I SAAC N EWTON G ROUP OF T ELESCOPES
Biennial Report 2004 2005 Published in Spain by the ISAAC NEWTON GROUP OF TELESCOPES (ING) ISSN 1575–8966 Legal license: TF–1142 /99
Apartado de correos, 321 E-38700 Santa Cruz de La Palma; Canary Islands; Spain Tel: +34 922 425 400 Fax: +34 922 425 401 URL: http://www.ing.iac.es/; http://www.ast.cam.ac.uk/ING/ (UK mirror)
Editor and designer: Javier Méndez ([email protected]) Preprinting: Gráficas El Time. Tel: +34 922 416 651 Printing: Gráficas Sabater. Tel: +34 922 623 555
Front cover: IC1396 or the Elephant Trunk Nebula. Image obtained as part of the Isaac Newton Telescope Photometric Hα Survey of the Northen Galactic Plane, and it was prepared by Nick Wright, University College London. Inset: Photograph of laser test on the William Herschel Telescope as part of GLAS preparatory study. Credit: Javier Méndez.
Other picture credits: Nik Szymanek (WHT, p. 4); Nik Szymanek (INT, p. 4); Nik Szymanek (JKT, p. 4); Nik Szymanek (ING, p. 5); Jens Moser (WHT, back); Jens Moser (INT, back); Nik Szymanek (JKT, back).
The ING Biennial Report is available online at http://www.ing.iac.es/PR/AR/ or at http://www.ast.cam.ac.uk/ING/PR/AR/. ISAAC NEWTON GROUP OF TELESCOPES
Biennial Report
of the PPARC-NWO-IAC ING Board
2004 – 2005 ISAAC NEWTON GROUP
William Herschel Telescope Isaac Newton Telescope
Jacobus Kapteyn Telescope
4 • ING BIENNIAL R EPORT 2004–2005 OF TELESCOPES
The Isaac Newton Group of Telescopes (ING) consists of the 4.2- metre William Herschel Telescope (WHT), the 2.5-metre Isaac Newton Telescope (INT) and the 1.0-metre Jacobus Kapteyn Telescope (JKT). The ING is located 2350 metres above sea level at the Roque de Los Muchachos Observatory (ORM) on the island of La Palma, Canary Islands, Spain. The WHT is the largest telescope of its kind in Western Europe.
The construction, operation, and development of the ING telescopes is the result of a collaboration between the United Kingdom, The Netherlands and Spain. The site is provided by Spain, and in return Spanish astronomers receive 20 per cent of the observing time on the telescopes. The operation of the site is overseen by an International Scientific Committee, or Comité Científico Internacional (CCI).
A further 75 per cent of the observing time is shared by the United Kingdom, the Netherlands and the Spanish Instituto de Astrofísica de Canarias. The remaining 5 per cent is reserved for large scientific projects to promote international collaboration between institutions of the CCI member countries.
The ING operates the telescopes on behalf of the Particle Physics and Astronomy Research Council (PPARC) of the United Kingdom, the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) of The Netherlands and the Instituto de Astrofísica de Canarias (IAC) of Spain. The Roque de Los Muchachos Observatory, which is the principal European northern hemisphere observatory, is operated by the IAC.
ING BIENNIAL R EPORT 2004–2005 • 5
TABLE OF CONTENTS
Foreword ...... 8 Introduction ...... 9
Chapters
1. Scientific Highlights ...... 10 2. Operation, Maintenance and Developments ...... 31 3. Use of Observing Time and Scientific Productivity ...... 37 4. In-House Research ...... 41 5. Public Relations ...... 47
Appendices
A. The Isaac Newton Group of Telescopes ...... 49 B. Telescope Instrumentation ...... 52 C. Staff Organisation ...... 53 D. Telescope Time Awards ...... 55 E. ING Bibliography ...... 64 F. Astronomy Staff Research Publications ...... 79 G. Seminars ...... 86 H. Financial Statement ...... 87 I. Committee Membership ...... 88 J. Addresses and Contacts ...... 89 K. Acronyms and Abbreviations ...... 90
ING BIENNIAL R EPORT 2004–2005 • 7 FOREWORD
It is a pleasure to write this foreword to the 2004-2005 Biennial Report of the Isaac Newton Group of Telescopes, on behalf of the ING Board.
The period 2004-2005 marks a new phase for the ING. The restructuring of the organization, prompted by a reduction in the level of funding, was completed in this period and at the end of this period the ING underwent a major review with a very positive outcome. These two aspects mark this period very well: despite the restructuring the ING has been able to maintain and develop a world class observatory with facilities that are high in demand and produce excellent science. The Board is very impressed with these accomplishments Prof. Thijs van der Hulst and wants to compliment the entire ING staff for carrying the observatory through harsh times in such an Chair of the ING Board effective way.
The participation of the IAC in the ING was very important for maintaining the funding of the ING at an appropriate level. In my opinion it has accomplished even more. It resulted in a more intensive collaboration between the different ING partners, which will prove to be invaluable for the future of the observatory at the Roque de Los Muchachos.
The past two years have been very productive from a scientific point of view. LIRIS, the near infrared imager/spectrograph designed and built by the IAC for the WHT, was commissioned successfully and has done exciting first science. As part of the NASA Deep Impact campaign it observed the collision between an impactor probe and the nucleus of comet 9P/Tempel1. Another new WHT instrument, OASIS, opened the area of high spatial-resolution imaging-spectroscopy. In combination with NAOMI, the adaptive optics system, it provides a unique capability for a wide range of interesting problems, ranging from the dynamics in the very centers of galaxies to spectroscopy of individual stars in star clusters or crowded regions. The laser guide star system that is now put together will open up the entire northern sky for AO assisted spectroscopy and imaging and bring to fruition a technical and science area that will prove to be very interesting and strategically important for both the ING and its communities.
But there was more: the demand for visiting instruments, all producing high quality science, remains higher than can be accommodated. The review panel recognized that the WHT is one of the few 4-m class telescopes that accommodates visiting instruments and considered this a very strong aspect in many respects: it produces excellent science and it maintains high quality instrument development within the community. The suite is quite impressive: PN.S, CIRPASS, INTEGRAL, SAURON, PLANETPOL and others to come.
The INT, now operational in a single instrument mode, as was the JKT before its retirement, continues to entertain excellent projects. Highlights are charting the environs of the Local Group galaxies Messier 31 and Messier 33 to unprecedented deep levels, the jet driven ring around Cygnus X-1 and the rings around planetary nebulae reflecting the mass loss history of the dying stellar precursor.
The Board started focusing its attention on the future of the ING past 2009 when the present contracts between the funding agencies NWO, PPARC and the IAC terminate. The high potential of the ING, in particular the WHT, is widely recognized. The ING community and the review panel have already made this clear, and we expect the funding agencies to come with positive formal statements soon. The pressure on funding in the presently participating countries is high and resources need to be shared with a several new initiatives in the realm of future large facilities. Yet the Board hopes, with the community that the funding agencies have the insight that maintaining a world class facility, even though consisting of modest size telescopes by modern standards, is crucial for the health of its scientific community.
8 • ING BIENNIAL R EPORT 2004–2005 INTRODUCTION
Welcome to the biennial report of the Isaac Newton Group of Telescopes for the years 2004 and 2005. The dynamics and excitement of astronomy have certainly been felt at the observatory during the last two years. As you can read in this report many scientific highlights passed the scene and important technical advances were made. This report provides an overview of the main events and summarizes the financial status and scientific output of the telescopes. The successes and achievements over the period covered by this report have only been possible thanks to the continued quality efforts of ING staff, who have shown a high level of commitment and professionalism through uncertain and sometimes difficult times.
It is now some thirty years ago that La Palma was being explored as a potential location for a new observatory Dr. René Rutten in the Northern hemisphere. That choice has most certainly paid off in scientific terms. The site testing Director of ING equipment in those days was not so sophisticated to today’s standards and the circumstances under which the work was conducted were rather primitive. The pictures below (courtesy of site tester Thomas Gough) give an impression of the situation. Although the observatory is now well established, characterization of the observing site continues and is even stepping up pace with the advent of adaptive optics, the construction of very large telescopes such as the 10m GTC, and the possibility of construction of a future Extremely Large Telescope. In the early days analysis of star trails and of sparse meteorological measurements were the basis for initiating the observatory; now we possess an arsenal of additional tool such as DIMM, MASS, SLODAR, and remote sensing to help us decide on the quality of the atmosphere. But what remains the same is the finding that La Palma is one of the very best observing sites in the World.
The reporting years saw also intense activity on growing European collaboration between observatories in which ING was strongly involved. Under the umbrella of OPTICON a large programme to promote trans- national access to telescopes was initiated. The demand for observing programmes for the ING telescopes was so large that limits had to be imposed to prevent the scheme from running out of resources. European collaboration, not only for the construction of future large facilities, but also for existing observatories will be beneficial to European astronomy at large. ING hopes to play a key role in this as well.
ING BIENNIAL R EPORT 2004–2005 • 9 Chapter 1
SCIENTIFIC HIGHLIGHTS
THE DISCOVERY OF A GALAXY-WIDE redshift has been less direct: it is unclear whether such SUPERWIND FROM A YOUNG outflows are localised to regions of intense star formation ≈ just a few kiloparsecs in extent, or whether they instead MASSIVE GALAXY AT REDSHIFT Z 3 have a significant impact on the entire galaxy and its surroundings. The formation of galaxies requires gas to cool in haloes of dark matter that collapse under gravity from the expansion To observe such outflows via absorption studies a of the Universe. However, cooling alone overproduces background light source is needed with a spatial extent bright galaxies at the present day, so models incorporate somewhat larger than a Lyman-break galaxy stellar body thermal conduction, photoionisation and galaxy merging, or a quasar sightline. Such a source is provided by the together with additional feedback in the form of galactic- recently discovered Lyman-α-emitting blobs (LABs), scale outflows. The latter are powered by supernovae and associated with Lyman-break galaxies in the SSA22 massive stellar winds, or by relativistic winds and jets resulting from gas accretion onto supermassive black protocluster at redshift z=3.09 (seen 11.5 gigayears ago holes. These high-velocity galactic outflows mark the when the Universe was 20 per cent of its current age), a termination of star formation in the most massive galaxies structure which is likely to evolve into a rich cluster of and deposit heavy elements in the intergalactic medium. galaxies. Sizes of these LABs are around 100 kiloparsecs and Lyman-α luminosities of about 1044 erg s-1. Although starburst superwinds have been studied in local dwarf galaxies, such as M82, observational evidence for The Lyman-α haloes of two of these LABs were observed their counterparts in young massive galaxies at high using integral-field spectroscopy, which, unlike conventional
Figure 1. Left: This shows the extent of the gaseous halo of LAB-2 (10 arcsec on the sky equates to a physical distance of 76 kpc in this galaxy approximately). The image was derived from observations with the SAURON Integral Field Spectrograph, by collapsing the data cube along the wavelength direction. The labels indicate regions for which one-dimensional Ly-α emission line profiles have been extracted and shown on the right. Right: Thick solid lines are fits to a model where the intrinsic Ly-α emission (dashed lines) is partially absorbed by foreground HI.
10 • ING BIENNIAL R EPORT 2004–2005 slit spectroscopy, gathers spatially resolved spectra over a is a strong signature of active stars, interacting binaries, two-dimensional area. Such information is essential for a very massive stars (especially supergiants, Luminous complete picture of the complex morphology of these Blue Variables and Wolf-Rayet stars), Be stars, post-AGB objects. Astronomers used the SAURON Integral Field stars, pre-main-sequence stars and so on. These objects Spectrograph on the William Herschel Telescope providing represent important evolutionary phases which are moderate resolution spectra over a 41 arcsec×31 arcsec generally short lived, and are hence few in number and area, sampled with 0.95-arcsec lenslets. difficult to find. Their discovery is therefore well worth the effort of a concerted programme and in August 2003 a Observations of object LAB-2 shows that its spatially major new survey project was started using the Wide Field extended Lyman-α line emission appears to be absorbed Camera (WFC) on the Isaac Newton Telescope (INT) to by neutral hydrogen in a foreground screen covering the do just that. It is called the INT Photometric Hα Survey of entire galaxy, with a lateral extent of at least 100 the Northern Galactic Plane, or IPHAS for short. kiloparsecs (over 300,000 light years across or about three times larger than the disk of our own Milky Way Its goal is to conduct an Hα survey of the entire northern galaxy) and remarkable velocity coherence. Based on the Galactic Plane in the latitude range –5°
Astronomers have long been puzzled about why key elements for the formation of planets and ultimately life (such as carbon, oxygen and iron) are so widely distributed throughout the Universe; only 2 billion years after the Big Bang, the remotest regions of intergalactic space have been enriched with them. The superwind observed in this galaxy shows how such blast waves can travel through space carrying the elements formed deep within galaxies.
THE ISAAC NEWTON TELESCOPE PHOTOMETRIC Hα SURVEY OF THE NORTHERN GALACTIC PLANE Figure 2. The crescent nebula, NGC6888, which surrounds the Wolf-Rayet star PPM 84423, seen in Hα emission by IPHAS. Hα emission is ubiquitous in our Galaxy. It traces ionised gas of assorted nebulae such as HII regions, planetary Figure 3. Next two pages: a 5°×3.5° mosaic of the supernova nebulae, Wolf-Rayet nebulae, and supernova remnants. It remnant S147 in Hα. North is to the top and East to the left.
ING BIENNIAL R EPORT 2004–2005 • 11
Figure 4. Filamentary Hα emission in Cygnus. The colour scheme Figure 5. Sh2-242 is a small HII Region on the edge of a molecular is red for Hα, blue for the Sloan r' band, and green for Sloan i' cloud that lies just southeast of the supernova remnant Simeis 147 band. As this is a significantly reddened region, as well as in the constellation of Taurus. There is evidence that this nebulous, there are many stars coming through strongly in the i' molecular cloud may contain a young stellar cluster of newly-born band, appearing here as a background of green stars. stars. Field of view is approximately 10×10 arcmin. North is down and East to the right.
Figure 6. The Pelican Nebula is a massive nebula in the constellation of Cygnus. It lies close to the North American Figure 7. Dust lanes in the centre of the Rosette Nebula. Field of Nebula, the two being separated by a giant dust cloud. This image view is 30×20 arcmin, north to the left, east is down. shows the main ionization front of the Pelican Nebula which makes up the head and neck of the Pelican. Recent observations have identified many new Herbig-Haro objects in this area, including two that can be seen in this image, the first on the far right hand side and the second at the end of the dust column in the second. Field of view is approximately 25×15 arcmin, North is to the left, East is down.
Figure 8. Sh 2-188 is a wind blown planetary nebula in Cassiopeia. It is a perfect example of a strong interaction between a planetary nebula and the interstellar medium. It shows a single arc-like structure with a faint, thin arc behind it. Also visible is a longer, wide arc extending away from the nebula itself. Recent studies have shown this shape to be due to the motion of the planetary nebula through the interstellar medium at a velocity of 125 km s-1. Field of view is 22 × 22 arcmin, North is up, East to the left.
14 • ING BIENNIAL R EPORT 2004–2005 Figure 10. NGC 6781 is a small bubble-shaped planetary nebula. It is approximately 2 light years across and shows some structure in the centre similar to that seen in the Helix Nebula. Field of view is 6×6 arcmin.
Figure 9. The newly discovered planetary nebula PN 126.62+1.32, the "Prince of Asturias" (named after the wedding of the Spanish Prince), is a rare quadrupolar nebula (central region), with Figure 11. Sh 2-71 is quite an irregular planetary nebula. The extended fainter lobes extending over 16 arcminutes from the central star is a variable star, and this may explain the strange central star. shape of the nebula itself. Field of view is 4×3 arcmin.
THE COMPANION STAR TO TYPE IA address observationally the identification of the surviving TYCHO BRAHE'S 1572 SUPERNOVA companion.
The brightness of type Ia supernovae, and their A team of astronomers carried out an imaging and homogeneity as a class, makes them powerful tools in spectroscopic survey using ISIS, UES and the Auxiliary cosmology, yet little is known about the progenitor Camera on the WHT of the central region of Tycho's systems of these explosions. They are thought to arise supernova remnant, around the position of the explosion. when a white dwarf accretes matter from a companion The analysis of the data excluded red giants as the mass star, is compressed and undergoes a thermonuclear explosion. Unless the companion star is another white donor of the exploding white dwarf. However, they found a dwarf (in which case it should be destroyed by the mass- type G0–G2 star, similar to our Sun in surface temperature transfer process itself), it should survive and show and luminosity (but lower surface gravity), moving at more distinguishing properties. than three times the mean velocity of the stars at that
Tycho’s supernova is one of only two type Ia supernovae distance, which they claim to be the surviving companion observed in our Galaxy, and so provides an opportunity to of the supernova.
ING BIENNIAL R EPORT 2004–2005 • 15 Tycho G is a star of type G0-G2 IV located at the distance THE LARGEST KNOWN PLANETARY of Tycho SNR and it moves in space at 136 km s–1, which is a factor of over 3 larger than the mean velocity of the NEBULA ON THE SKY surrounding stars (Tycho G’s metallicity in Fe and Ni are The vast majority of Planetary Nebulae in our own Galaxy similar to solar values and therefore it can´t be a halo star). have been identified via wide-field narrow-band Hα Its low surface gravity can also be interpreted as a surveys or through wide-field low-resolution slitless consequence of mass stripped by the impact of the spectroscopic surveys, with both techniques attempting to supernova explosion. isolate objects showing very high equivalent width emission lines that are characteristic of PNe.
Examining the results of an automated search of the Sloan Digital Sky Survey (SDSS) spectroscopic database for emission lines from putative high-redshift sources, one particular galaxy showed an unambiguous emission line detection with a somewhat weaker feature to the blue. The emission line pair was immediately identifiable as emission from [OIII] 4959, 5007. Not an entirely unexpected occurrence but the unusual feature of the detection was that the wavelength of the detection placed the emission at essentially zero radial velocity. Querying the output of the emission line search for similar detections produced more spectra showing a similar signature. All of the objects possessing [OIII] emission occurred in an approximately circular region with a Figure 12. Centre of Tycho's supernova remnant (Tycho SNR). diameter of ~1.5°, with not a single detection anywhere The star marked as 'G' is the one identified as the companion star of Tycho Brahe´s 1572 supernova. Since the supernova explosion else on the sky. Investigation of SDSS spectra of stars, in 1572, Tycho G has moved 2.6 arcseconds south on the sky. quasars and even sky fibres revealed further detections, all concentrated in the same region of sky.
A series of checks fairly rapidly eliminated the majority of instrumental artifacts or transient phenomena as the cause of the emission. Combining spectra beyond the boundaries of the region where [OIII] emission was detected produced clear detections of [OIII] emission extending over a region more than 2° in diameter. A smaller number of individual spectra also showed the presence of emission from Hα and [NII] 6548, 6583. The spatial distribution of the individual emission line detections revealed clear trends and composite spectra, made up from objects contiguous on the sky, confirmed the trends and even allowed the detection of [SII] 6718, 6732.
Narrowband imaging of the central part of the region was carried out using the WFC on the INT. The results were unambiguous, with excellent agreement between the surface brightness distribution evident in the INT images Figure 13. The spectra shown here are of the candidate star for and the emission line detections from the SDSS spectra. the companion to SN 1572 (Tycho G), a red giant (Tycho A) and A striking feature of the images was the presence of a main-sequence star (Tycho B). Spectra were obtained at the WHT well-defined arc-like feature, perhaps suggestive of some with UES and ISIS. The upper panel shows the observed spectrum near Hα. This line is blueshifted, implying a peculiar radial velocity form of shock. A search of the region using SIMBAD exceeding about 3 times the velocity dispersion for its stellar type. revealed the presence, close to the region with the
16 • ING BIENNIAL R EPORT 2004–2005 Figure 14. The left hand panel shows a mosaic of 6 INT WFC continuum–subtracted pointings in Hα+[NII] while the right panel shows the equivalent for [OIII]. The images are approximately 0.8° on a side with North to the top and East to the left. The location of the white dwarf PG1034+001 is indicated by a circle in the [OIII] image. Emission with complex structure is evident in the central regions of the images in both passbands. A well–defined arc, or boundary, is visible at center–right in the [OIII] image. strongest [OIII] emission, of a very nearby, extremely hot 87 days after explosion. A team of astronomers also DO white dwarf (PG 1034+001). The location of the white observed its gradually fading light for several months dwarf clinched the identification of the emission region as using the INT. a PN. The progenitors of type II-P SNe have long been thought The diameter of more than 2° makes the object the largest to be red supergiant stars with initial masses greater than known PN on the sky. The spectroscopic distance 8 to 10 solar masses that have retained their hydrogen estimate of 155+58 pc means the PN is certainly the envelopes before core collapse. This model accounts for second closest known and a parallax distance could the 2- to 3-month-long plateau phases seen in the confirm the nebula as the nearest PN to the Solar System. lightcurves of SNe II-P, the existence of hydrogen P-Cygni The unambiguous detection of a PN associated with a profiles (which are indicative of an optically thick non-DA white dwarf is also a first. The PN is certainly old, expanding atmosphere) in the early time spectra, and the an estimate of the expansion age and a kinematic age estimated physical parameters of the expanding estimate, derived from extrapolating the observed proper photosphere such as velocity, temperature, and density. motion of PG 1034+001 back to the origin of the radius of Stellar evolutionary calculations are consistent with this curvature of the arc feature, both suggest an age of picture, in which stars with initial masses in the range of 8 ~100,000 years. The strongly enhanced [NII] emission to 25 solar masses reach the end of their nuclear burning evident along the south western boundary of the PN is lives when they are red supergiants. also indicative of the interaction of an old PN with the surrounding interstellar medium. Only two progenitors of unambiguous SNe have been directly identified and yielded estimates of luminosity, FIRST DETECTION OF A PROGENITOR temperature, and mass. These are the progenitors of the peculiar type II-P SN 1987A, which was a blue supergiant, STAR FROM A NORMAL TYPE II-P and the IIb SN 1993J that arose in a massive interacting SUPERNOVA binary system. The expected red supergiant origin for the common type II-P SNe has so far eluded direct detection. Supernova 2003gd was discovered on 12.82 June in the The fortuitous coincidence of a type II-P SN occurring in a nearby spiral galaxy M74. From observations carried out nearby galaxy that has high-quality prediscovery images using the ISIS spectrograph on the WHT, it was shown to available has allowed the direct determination of the be a type II–plateau (II-P) SN that was discovered about physical parameters of a SN progenitor for only the third time.
ING BIENNIAL R EPORT 2004–2005 • 17 Figure 15. Isaac Newton Telescope image of M74 (NGC 628) with inset (top) showing pre-explosion star (enhanced) from a Gemini image and (bottom) SN2003gd after it exploded from Isaac Newton Telescope when the supernova was 6 months old.
The galaxy M74 was observed with the HST about 200 progenitors of three nearby type II-P SNe by the same days before the estimated explosion date of SN 2003gd of method as followed with SN 2003gd. Although these have 18 March 2003 (with an uncertainty of about 21 days). failed to detect an object, they have been able to set This galaxy was also observed about 310 days before the restrictive upper mass limits. Mass limits of the progenitors explosion by the Gemini Telescope. An approximate were estimated to be 15 solar masses for SNe 1999em position for the SN was estimated from images obtained and 2001du and 12 solar masses for SN 1999gi. These using the Auxiliary Port Camera of the WHT and precise three SNe and 2003gd are all spectroscopically very similar differential astrometry from HST images. Astronomers and appear to be a common, homogeneous class of type II. identified an object in the pre-explosion HST and Gemini images that is coincident with SN 2003gd. Stellar evolutionary models and theories of the SNe lightcurve and spectral evolution have long predicted that This is the first detection of a progenitor star from a normal red supergiants should be the progenitors of SNe type II-P. type II-P SN, which is the most common type of SN (by volume) in the Universe. It is a red supergiant, which is However, there is a quantitative discrepancy now consistent with the models of single stellar evolution. appearing between the masses that have been derived for Recently, there have been attempts to identify the these four SNe II-P and the mass required to support the
18 • ING BIENNIAL R EPORT 2004–2005 long plateau phase with normal expansion velocities. Consistently high ejecta masses have been derived for a large sample of 13 SNe II-P in the range of 17 to 56 solar masses, quite different from the low masses that the direct method suggests. However, the three SNe with excellent monitoring data and direct mass limits do show agreement, which is strong evidence that the common type II-P SNe originate in stars with masses between 8 and 15 solar masses.
A PANORAMIC DEEP VIEW OF THE STELLAR HALO OF ANDROMEDA GALAXY
The structure of the outer regions of galaxies is a key area in which to look for fossil remnants of the accreted masses from which the galaxies that we see today are thought to be built. The importance of these regions has increased in recent years as cosmological theories of structure formation become more exact in their predictions, and the observational instrumentation required to conduct these detailed analyses becomes more sophisticated. Figure 16. A multi-colour mosaic of the INT WFC survey of M31, involving 165 individual pointings over 40 square degrees of the Currently composed of 165 individual pointings of the INT sky, which shows the inhomogeneity of this system. Metal- poor/young stars are coded blue whilst metal rich/older stars are Wide Field Camera (WFC), the M31 halo survey consists coded red. The (colour-dependant) substructure is obvious, and of photometry for over 7 million sources, on a photometric surprising given the pristene nature of the Galactic disk. The dwarf system accurate to 2% over ~40 square degrees on the galaxies Andromeda I & III are visible at the bottom left of this sky, in some places probing the halo of Andromeda out to figure; the newly discovered dwarf spheroidal, Andromeda IX, is just visible at the top left as a small blue dot. NGC 205 is also 6° (~80 kpc). Observations of 800–1000 seconds in the visible in this figure, at the right-hand side of the disk This Johnson V (V') and Gunn i (i') passbands are deep enough spectacular image shows in amazing detail the wealth of to detect individual RGB stars down to V'= 0 and Main information that the INT is helping to reveal about the structure of Sequence stars down to V'=–1. This unique dataset has this previously invisible region of galaxies. provided, for the first time, a panoramic deep view of the stellar halo of a giant galaxy thought to be similar to our A second large stellar stream candidate has also been own Milky Way. identified with the INT WFC photometry. The visible part of this feature is some 15 kpc long. The progenitor of this Despite exhibiting a near pristene disk, M31’s halo is full feature appears to be the satellite galaxy NGC 205. This of substructure and points to a history of accretion and object has long been known to be tidally perturbed but it is disruption. The most obvious piece of substructure is the only now that the full extent of its disruption is becoming giant stellar stream (visible in the south-east). This clear. Considerable amounts of other substructure exists extends to near the edge of the survey — a projected in addition to these streams. distance of some 60 kpc. In fact, by examining the systematic shift in the luminosity function of the stream as The other spiral in the Local Group, the Triangulum Galaxy a function of galactocentric radius, a length much greater (M33), has also been surveyed with the INT WFC. The than 100 kpc is found. The similarity of the colour of this structure of this galaxy is striking in comparison to M31: feature with the loop of material at the north of the survey the lack of substructure is immediately obvious. It appears suggests it seems likely that the northern feature is an that not all spiral galaxy haloes need look like M31. There extension of the stream, after it has passed very close to is then the question of the M31 dwarf satellite galaxies. the centre of the potential of M31. The homogeneous nature of the data has allowed
ING BIENNIAL R EPORT 2004–2005 • 19 between (negligible dark matter) classical globular clusters and (dark matter dominated) dwarf spheroidals, and are unlike any clusters found in the Milky Way, or elsewhere to date.
The fields visually investigated included the whole INT Wide Field Survey of M31, an area far into the halo, and an additional region south along the Andromeda Stream, and towards M33, making a total area of more than 40 2 Figure 17. The distribution of the satellite galaxies of M31, as deg . The survey consisted of V’- and Gunn i’-band derived from the INT WFC photometry of these objects. The images reaching limiting magnitudes of i’=23.5 and coordinate system is an M31–centric system. The plane is the V’=24.5, and taken in average seeing of 1.2 arcsec. These plane of the disk of M31, and each cell corresponds to 100 images were processed by the INT-WFS pipeline provided kpc×100 kpc. l is a longitude measured around the disk of M31, by the Cambridge Astronomical Survey Unit, which such that l=0 is the longitude of the Galaxy. b is a latitude, measured from the disk of M31. Solid lines indicate objects includes tools for astrometry, photometry and object located above the plane of the disk, while dashed lines indicate description and classification. objects below the plane of the disk. A clear tendency for the satellites to lie on the near side of M31 can be observed, and The extended M31 clusters have no known analogues in suggests an intriguing correlation between the M31 satellites and the Milky Way, where such clusters would certainly have our own Galaxy. been discovered if they existed, unless hidden by the plane of the Galaxy. This suggests that they could hold accurate and internally self-consistent distances and important clues to the differing formation histories of these metallicities to be measured for each of these galaxies. galaxies. If these clusters were not born with their present For the first time, the three dimensional spatial distribution morphology then one may speculate that they are the of these objects, has reliably probed and revealing that far stripped cores of cannibalized dwarf spheroidal galaxies, from being isotropically distributed and unbiased or the products of cluster mergers perhaps themselves indicators of the potential of Andromeda, there are strong created in a previous interaction of a gas-rich companion indications that these objects are preferentially located on with M31. the near side of Andromeda, towards the Galaxy. RINGS IN THE HALOES OF A NEW POPULATION OF STAR PLANETARY NEBULAE CLUSTERS IN THE HALO OF M31 The end-point of the evolution of solar-type stars is As part of the INT WFC survey of M31, a search for essentially determined by the onset of a strong stellar globular clusters in a large part of the halo has been wind, which, in a few hundred thousand years completely carried out. Globular clusters systems are valuable tools removes the star’s gaseous envelope, thereby removing for the study of the evolution of their host galaxies, acting the fuel that has previously maintained the thermonuclear as chemical and dynamical probes. Specifically, most energy source in its interior. This phenomenon occur during globular clusters are believed to be old objects, and thus a (second) phase in which the star becomes a red giant, the provide clues to the earliest epochs of galaxy formation so-called the Asymptotic Giant Branch (AGB) stage. In the history. last million years of the AGB, the red giant is dynamically Three extended, luminous globular clusters were unstable and pulsates with typical periods of few hundred discovered during this search for classical clusters. days: a prototypical star in this phase is Mira in Cetus. The Although having globular-like colours and luminosities, mechanical energy of the pulsations pushes large they have unusually large half-light radii, ~30 pc amounts of material far away enough from the core of the (compared to typical values between 1 and 7 pc) and they star for it to cool down and condense into dust. This newly are hundreds of times less dense — the distances formed dust is further accelerated out of the gravitational between the stars are, therefore, much greater. They lie at bounds of the star by the pressure of the radiation coming projected galactocentric distances of ~15 to ~35 kpc. from the hot stellar remnant. Gas, which is coupled to dust These objects begin to fill the gap in parameter space by collisions, also leaves the star in this process.
20 • ING BIENNIAL R EPORT 2004–2005 Figure 18. The location of the new extended globular clusters in relation to major landmarks of the M31 system (open circles), and the survey area (red dotted outline). The ellipses represent a 2° radius disc aligned and tilted to the inclination of M31 and an oblate halo of axial ratio 0.6 aligned along the major axis. The kpc scales correspond to a distance to M31 of 780 kpc. To the right, V- and i-band images of the new luminous 'extended' clusters, from the INT–WFS images. Each image is 1 × 1 arcmin2, with north up and east to the left. Cluster 3 is a partial image as it lies on the edge of an INT–WFS field. Right: Images of two of the newly discovered clusters. Below them are examples of M31's normal globular clusters, which have similar luminosities but whose stars are much more concentrated together (and hence the images of the globular clusters are saturated in the centres of the clusters).
In the last hundred thousand years of the AGB, this mass loss process is so strong that the star is completely surrounded by a thick, expanding dust shell that makes it very difficult to observe what is going on inside it. One way to recover valuable information about this critical phase of stellar evolution is to study the progeny of AGB stars, i.e. planetary nebulae (PNe). These are nothing but the ejected AGB envelopes, heated by the radiation of the hot stellar core, and therefore emitting at the specific wavelengths (emission-lines) typical of the gas that they are composed of.
PNe are fantastic laboratories in which to study a variety of physical phenomena, for example, in the past many aspects of atomic and molecular physics have been addressed by studying PNe. More recently, PNe have become laboratories for investigating the (hydro)dynamical formation of shock waves produced by collisions between stellar winds, with the consequent Figure 19. Images of rings recently detected in PNe using the INT formation of thin gaseous shells, and bipolar flows or jets WFC. Left: [OIII] images. Right: the same images processed to enhance the rings. which closely resemble those observed in other type of stars or in the nuclei of active galaxies. If we understand pulses at about 1500 years intervals during the last 20,000 the formation of the complex and spectacular shapes years of the AGB evolution. Each shell contains about one displayed by PNe, a lot can also be understood about the hundredth of the mass of the Sun, i.e. approximately the very late AGB evolution. mass of all the planets in the Solar System combined. When projected in the sky, these shells appear as “rings” An observational highlight in the investigation of the (or sometimes “arcs”) composing a sort of “bull’s-eye” pattern. shapes of PNe came from the HST images of the Cat’s Eye, which revealed the presence of a series of shells in Discovery of these rings came as a surprise, as mass-loss the inner regions of its halo. They appeared to be modulation on a timescale of 1000 years was not produced by mass ejected from the star in a series of predicted by theory (compare with the 100 times longer
ING BIENNIAL R EPORT 2004–2005 • 21 timescale of the recurrence of thermal pulses). First, it was spacecraft flybys. Deep Impact was designed to provide a thought that rings were a rare phenomenon, but recent first look at the interior of a comet by striking the surface observations taken mainly with the Wide Field Camera of to expose the material underneath the opaque crust. the INT, have instead shown that these structures are likely the rule rather than the exception. They are thus of The target comet was comet 9P/Tempel1. This is one of a general relevance to understanding the large mass loss class of comets known as the Jupiter-family of comets, increase that characterises the end of the evolution of a most of which are believed to have formed in the trans- star like the Sun. Neptunian region. These objects have low inclination orbits and typically take less than 20 years to orbit the Several mechanisms have been proposed for the Sun. Their orbits are strongly influenced by Jupiter, hence formation of these rings. They include binary interaction, their name. 9P/Tempel1 orbits the sun once every 5.5 magnetic activity cycles, or stellar pulsations caused by years, and the Deep Impact encounter was scheduled to instabilities in the hydrogen burning shell inside the AGB take place at perihelion, when the comet was at 1.5 and envelope. Another possibility is that gas is ejected 0.9 Astronomical Units from the Sun and Earth, smoothly from the star, and rings are created later on due respectively. to formation of hydrodynamical waves in the outflowing material that are caused by a complex coupling between Deep Impact was designed so that much of the mission- gas and dust. In any case, it is clear that any AGB mass critical science would be done from Earth-based loss theory should now confront the evidence that these telescopes. These facilities would observe the comet rings are frequently found in PNe, and thus contain before, during, and after impact. This was an important information relating to the very late evolution of unprecedented coordinated observational campaign, a large fraction of stars in the Universe. which included over 550 whole or partial nights of observation using 73 ground-based telescopes at 35 THE DEEP IMPACT EVENT AT THE observatories. These facilities would observe the comet’s evolution in wavelength regimes and timescales ING TELESCOPES inaccessible to the spacecraft.
The NASA Deep Impact mission was due to collide with a The Roque de Los Muchachos Observatory played a comet in order to reveil the composition and constitution of substantial role in this campaign. Observations started in comets and thereby provide better insight into these 2000. But the interesting part of the game started on July bodies that go back to the early phases of the formation of 2nd, 2005. From July 2nd to July 10th a campaign the Solar System. The mission consisted of two involving three telescopes of the observatory, the WHT, spacecrafts: an impactor, weighting 364 kg, and a flyby the TNG and the NOT was conducted. LIRIS at the WHT spacecraft for observing the impact and relaying data from was used from July 3rd to 7th to obtain near infrared the impactor. The main goal of the mission was to study images in the J and K bands and near infrared spectra. the interior and outer layers of a comet. Until the impact, Also another group used the INT and the Liverpool very little was known of the internal structure and the Telescope to follow the activity of the comet from July 1st physical evolution of the outer layers of a comet nucleus. to 7th. The five largest telescopes of the Roque de Los Most of what we know relies primarily on theoretical Muchachos Observatory were used simultaneously to models. The relationship between the coma’s composition track an astronomical experiment in an unprecedented way. and the nucleus composition is also uncertain. Even if the coma is formed by material from the nucleus, there are On July 3rd, 2005 the Deep Impact impactor probe several physical and chemical processes that rapidly successfully separated from its mother craft onto a affect the material ejected from the nucleus. trajectory that would plunge the probe into the nucleus of comet 9P/Tempel1 at a velocity of 10 kms–1. At 05:44:36 Comets are remnants of the early stages of the formation UT on July 4th the impactor collided with the comet of our Solar System and thus contain the most pristine producing an impact of 19GJ of kinetic energy and material from that era, as well as clues to its subsequent excavating a crater shaped by gravity. evolution. Whatever evidence we have into their internal composition comes either from remote observation and The first aim of the campaign was to study the dust ejected modelling of the dust and gases that are lifted off the by the impact by using the high S/N images obtained in the surface, or from in-situ analysis of data from recent visible and near infrared, and the spectra in the near
22 • ING BIENNIAL R EPORT 2004–2005 Figure 20. First row: Sequence of calibrated near-infrared J-images of the dust coma of comet Tempel1 obtained with LIRIS at the WHT. Notice the changes in the images from July 3rd (pre-impact) to July 4th (taken 16 hours after the impact). Second row: Post-impact J- images processed to show only the dust ejected by the impact. Each image has been divided by the pre-impact one obtained on July 3rd. The evolution of the ejecta cloud is clearly seen. Third row: Same as 2nd row shown in a different flux scale.
Figure 21. These dramatic images of the expanding and dissipating ejecta plume were obtained by dividing the July 4th, 5th, and 6th coadded images of the comet by the pre-impact image on July 3rd. North is up and East to the left. The plume expands mostly into the South-Western quadrant, and appears to be decelerating at a non-uniform rate. The dust particles at the leading edge of the plume, are expanding at a rate of ~210 ms–1 (±10%) on July 4th (measured at a Position Angle of 225°). The field of view in every image is 190×190 arcsec, which is equivalent to ~123,000×123,000 km at the comet. infrared where there are many features due to gas The impact produced an ejected cloud of dust and the emission. The evolution of the intensity and colour of the observers were able to obtain a set of excellent images, in dust gives important information on the size of the ejected particular, in the R and J bands. At these wavelengths the grains, like their size distribution and ejection velocities. images were sampling the reflected sunlight by the dust in The second aim of the campaign was to measure possible the coma. The spectra also showed that the gas variations of the gas emission by means of visible contribution was very low in particular in the near infrared. spectroscopy, to detect any possible new activity in case Some conclusions about the dust cloud ejecta follow: the the impactor penetrated deep enough to meet the fresh dust ejected by the impact formed a semi-circular ices below the dust mantle. This would evaporate part of expanding cloud that extended from position angles (PA) them and expose ices to the sun-light generating a new 145° to 325°; assuming an albedo typical of cometary active area. grain size, and from the flux of the dust ejecta, an
ING BIENNIAL R EPORT 2004–2005 • 23 Figure 22. When comet Tempel1 came into view from La Palma, some 16 hours after the Deep Impact probe struck the comet, observes were able to start tracking the target comet with the INT. Both images above are a combination of 7×20 second Sloan- Gunn r' (red) filter images which isolate the dust component of the coma. The image on the left was taken on July 3rd between 21:56 and 23:03 Universal Time, about 7 hours before impact. The image on the right was taken between 22:08 and 23:56 UT on July 4th, 16 hours after probe impact. The comet was seen to increase in brightness by a factor of two —as measured in the central pixel— before and after the impact as seen from this location. Even in these images the effects of the impact can be seen by the changing coma shape between the two images. North is up and Figure 23. Larson-Sekanina image processing techniques were East to the left. The field of view in both images is 340×340 applied to the coadded r'-filter coma images from four of the nights arcsec, which is equivalent to ~220,000×220,000 km at the comet. to reveal the dramatic changes in the structure of the dust coma that resulted from the impact. Before impact on July 3rd (upper left estimation of a total mass of dust ejected of ~106 kg panel), three jet structures can be seen to be emanating from the comet’s nucleus. On July 4th, just 16 hours after probe impact, the (equivalent to about 10 hours of normal comet activity) can intensity of the jet/coma structures in the West and Southern be derived; the orientation of the ejecta proves that the direction increase dramatically (upper right panel). North is up and impact happened below the orbital plane of the comet; the East to the left. On July 5th, new curved structures can be seen in position of the leading edge of the dust cloud present on the North-Western quadrant (lower left panel), possibly made the July 4th images show that it expanded outward at a visible by the extra material ejected into the coma from the impact. projected speed of about 200±20 ms–1 (though varying The structures seem to return to their pre-impact status on July 6th (lower right panel). The field of view in every image is 95×95 with azimuth). arcsec, which is equivalent to ~62,000×62,000km at the comet.
In the following days the shape of the cloud changed because of the effect of solar radiation pressure that Kea, Hawaii. The observing slot ran from July 1st to July moved the dust particles to the tail of the comet (PA=110°). 7th, 2005. A period which overlapped the Deep Impact The maximum projected distance in the sunward direction, encounter allowed the observers three nights pre-impact achieved on July 7th, was 30,000 km. By July 9th most of and four nights post impact observing. The strategy was to the ejected dust was moved to the coma and the comet use the Wide Field Camera to obtain image mosaics up to looked like as in the pre-impact phase. The ejected dust is 5 million kilometres along the projected anti-solar direction diluted in the comet tail. to look for ion-tail features that may have been produced as a result of the impact. The study of the structures of the dust coma in high S/N images provided also very interesting results. The comet The post impact observations quickly revealed that no presented some dust structures in the pre-impact phase such ion features were present, which was subsequently that indicate that the nucleus had some particularly active confirmed by other observers performing similar regions. These structures remained after the impact, thus programs. With this in mind it was decided to focus on these active regions were not affected. And the new deep optical imaging of the central gas and dust coma structures observed after the impact on July 4th rapidly through UBVr'i'O+ filters. When the comet was imaged on disappeared and none remained at a high S/N level after July 4th, about 16 hours after the impact, the comet was a few days. seen to have increased in brightness by a factor of two — The observations from the INT were very important for as measured in the central pixel— compared to the July completing the time base coverage of the comet as it fell 3rd pre-impact levels. Some dramatic changes were seen below the sky from the primary observing site at Mauna in the dust coma. The Deep Impact event did not create a
24 • ING BIENNIAL R EPORT 2004–2005 new period of sustained cometary activity, and in many radio lobes associated with jets from AGN are commonly ways the artificial impact resembled a natural outburst. used as accurate calorimeters of the power×lifetime product of the jets, a method only very recently applied to In conclusion, the impact was an impulsive event that jets from stellar mass black holes. affected the dust mantle of the comet. A large amount of dust was ejected into the coma in a very short time. In no In 2004, very deep low radio frequency observations of the more than 5 days this dust dissipated. Also, if the impactor field of Cyg X–1, a 10-solar-mass black hole, resulted in reached the fresh-ices below the dust mantle, it did not the discovery of a shell-like structure which is aligned with excavate enough to expose a sufficient amount of ices to the resolved radio jet of this BHXB. This radio shell has create a new region sufficiently active to be easily detected. been interpreted as the result of a strong shock that develops at the location where the collimated jet impacts A JET-POWERED BUBBLE FORMED IN on the ambient ISM. Models of jet-ISM interactions predict a shell of shocked compressed ISM visible via THE GAS AROUND BLACK HOLE bremsstrahlung emission, containing a bubble of CYGNUS X-1 relativistic synchrotron-emitting plasma. The spectrum of the shocked shell should be approximately flat from radio Galactic black holes undergoing accretion are thought to to much higher frequencies and possess spectral lines in emit the bulk of their power in the X-ray band by releasing emission. To test this, the Cyg X–1 jet-blown nebula was the gravitational potential energy of the infalling matter. At consequently observed at optical wavelengths with the the same time, they are capable of producing highly Wide Field Camera of the INT. collimated jets of energy and particles flowing out of the system with relativistic velocities that travel into the The shell of the nebula is clearly visible in a 100-minute surrounding medium. Hα image (a lower limit of m=23.1 arcsec–2 from the nebula was calculated from the observations). The Black Hole X-ray Binaries (BHXBs) are the essential researchers claim that an emission mechanism with a flat laboratories for understanding the overall physics of the spectrum, such as bremsstrahlung, plus excess flux accretion process in these systems, and have provided us possibly due to line emission, as expected in the case of with a wealth of understanding of, for example, the radiative shock, can explain the radio and optical data properties of the accretion disc. In comparison, the energy obtained. However, the spectrum is inconsistent with that and matter content of the jets produced by BHXBs are not of optically thin synchrotron radiation. This, therefore, is well constrained because they are radiatively inefficient. the first detection of a thermal shell of gas that is shocked by its interaction with a jet of a Galactic black hole. Relativistics jets are a common feature of accreting black holes on all mass scales, ranging from supermassive The discovery of this large-scale (~5 parcsecs in diameter) black holes at the centres of active galactic nuclei to ring-like structure surrounding Cygnus X-1 that appears to stellar-mass black holes in X-ray binary systems within our be inflated by the inner radio jet, imply that low-luminosity own Galaxy. Whereas the inflow of hot gas can be very stellar-mass black holes as a whole dissipate the bulk of efficient in producing light (up to 40% of the accreted the liberated accretion power in the form of "dark", material may be transformed into energy and radiated radiatively inefficient relativistic outflows, rather than away in the form of optical/ultraviolet/X-ray photons), the locally in the X-ray-emitting inflow, whose key signature is same is not true for the synchroton-emitting outflow, the eventual energization of the ambient medium. So for whose efficiency might be lower than a few per cent. decades astronomers have been severely Estimating the total — radiated plus kinetic — power underestimating how much power black holes pump back content of the jets, and hence their importance with into the universe instead of merely swallowing material respect to the accretion process in terms of energetics, is across their event horizons. a primary aim of high energy astrophysics. The discovery team ruled out the possibility that the ring Attempts at measuring the jet power from radio might be the low-luminosity remnant of the supernova that luminosities are riddled with assumptions about its spawned the black hole. Since Cygnus X-1 moves in the spectrum and radiative efficiency. However, the jet power sky along a trajectory that is roughly perpendicular to the can also be constrained by analysing its interaction with jet, it cannot possibly have been located in the centre of the surrounding interstellar medium (ISM). Synchrotron the ring.
ING BIENNIAL R EPORT 2004–2005 • 25 means that optical searches for such SNe are unlikely to be successful.
By observing in the near-IR Ks-band the extinction is strongly reduced, making searches for such dust obscured SNe look feasible. Making use of this advantage, astronomers have been carrying out a near-IR Ks-band search campaign for SNe obscured by dust in the nuclear regions of nearby starburst galaxies with the WHT since 2001. Initially, the search started using INGRID near-IR imager. In 2004 observations with LIRIS commenced. By that time, the search had only produced the detection of a possible SN in old images making any follow-up observations and definite confirmation of this SN impossible. They estimated that the lack of SN detections from the INGRID SN search database indicated an average extinction towards the nuclear SNe exceeding
AV=10. Such high extinctions would certainly be expected for most of the SNe within the nuclear regions of starburst galaxies such as M82. Figure 24. The 100-minute Hα exposure obtained with the INT WFC of the field of Cyg X–1 (the black hole is depicted by the Already on the first run LIRIS observed a SN, SN 2004am, cross on the bottom-left) and the ~5.5 arcmin jet-blown nebula. 3σ radio contours are overplotted in white. within the nuclear regions (~500 pc) in M82. The discovery of this event, however, had already been reported just one µ This profitable technique has potential for constraining the day before the observations. The 0.89-1.53- LIRIS jet power associated with other BHXBs if further jet-blown spectrum showed broad hydrogen lines demonstrating that this was a type II event. The LIRIS JHKs images nebulae are identified. With the confirmation of this jet-ISM showed a moderately reddened source exactly coincident interaction associated with Cyg X–1, it is clear not only with a bright starburst knot within the nuclear regions of that there may be an undiscovered population of jet-blown M82. The optical-near-IR colours also showed that the bremsstrahlung nebulae associated with BHXBs, but also extinction towards this SN was AV~5. that these nebulae may easily be found with simple wide- field red-optical imaging. Later observations with LIRIS in 2005 produced discoveries of subsequently confirmed SN events in the HIGHLY ATTENUATED SUPERNOVAE interacting luminous infrared galaxy Arp 299 (distance ~45 Mpc) and in the nearby starburst galaxy NGC 2146 IN THE NUCLEAR REGIONS OF (distance ~13 Mpc). Both Arp 299 and NGC 2146 have STARBURST GALAXIES high expected CCSN rates of ~1–2 and ~0.2 SNe per year, respectively, as indicated by their far-IR luminosities. A handful of nearby supernovae (SNe) with visual SN 2005U with Ks=16.2 was discovered 1.3 kpc from the extinctions of a few magnitudes have recently been Ks-band nucleus A of Arp 299 and it was classified as a discovered. However, an undiscovered population of type II SN. The near-IR colour estimated from the LIRIS images gave an extinction of AV~4. SN 2005V was also much more highly attenuated (AV>10) core-collapse discovered by LIRIS on the same night. It had a magnitude supernovae (CCSNe) is likely to exist in the nuclear of Ks=13.8 and it was located 330 pc from the Ks-band (central kiloparsec) regions of starburst galaxies. For nucleus of NGC 2146. It was spectroscopically classified instance, in the nuclear regions of M82 and other nearby as a type Ib/c SN, about 1–2 weeks past maximum starburst galaxies one core-collapse supernova is brightness. The near-IR colours from LIRIS indicated an expected to explode every 5–10 years. Furthermore, in extinction of AV~3–4 towards SN 2005V. luminous infrared galaxies (LIRGs) such as the interacting system Arp299 (NGC 3690+IC 0694) at least one CCSN The combined INGRID and LIRIS SN search database can be expected every year. The high dust extinction includes images for 40 nearby starburst galaxies, on
26 • ING BIENNIAL R EPORT 2004–2005 Figure 26. JKs LIRIS image of Arp 299 (+SN 2005U) observed on 2005 Jan 30.
Figure 25. Top: JHKs LIRIS image of M82 (+SN 2004am) observed on 2004 Nov 25. Bottom: The result of alignment, image matching and subtraction between LIRIS Ks band images from March 2004 and November 2004. Note that by this time the SN Figure 27. JHKs LIRIS image of NGC 2146 (+SN 2005V) had already dimmed considerably. observed on 2005 Jan 30. average observed ~4.3 epochs per target. Although A recent deep neutral hydrogen survey of the Virgo several CCSNe have now been discovered in starburst Cluster (VIRGOHI) using the multibeam system on the galaxies at near-IR wavelenghts, they are all extinguished Lovell Telescope has covered 32 deg2 and detected 31 by only a few magnitudes in AV. The expected population sources, of which one of them, VIRGOHI 21, does not of highly extinguished supernovae within the nuclear have an optical counterpart. There have been several regions of starburst galaxies therefore still remains previous claims of the detection of isolated clouds of unrevealed. extragalactic gas with no stars in them, but subsequent analyses have either revealed the optical counterparts or A DARK HYDROGEN CLOUD IN THE shown that the gas is mereley debris from nearby visible VIRGO CLUSTER galaxies. Many other detections of HI clouds have been associated with nearby optically bright galaxies, but Simulations of cold dark matter models predict far more VIRGOHI 21 cannot be so easily explained. dark matter halos than are observed as galaxies. For this reason, it has been hypothesized that there must exist Following detection, VIRGOHI 21 was observed at the dark matter halos that contain no stars. The advent of Arecibo Telescope and the Very Large Array (VLA). From neutral hydrogen multibeam systems has allowed surveys the HI flux astronomers calculated an HI mass of 108M of large areas of sky to be carried out with much higher solar ∆ -1 sensitivity than has been possible in the past, thus and a velocity width of V20=220 km s . From the speed it allowing sources to be detected by their gas content alone is spinning VIRGOHI 21 is a thousand times more rather than their stars and opening up the possibility of massive that could be accounted for by the observed finding truly isolated clouds of extragalactic gas with no stars. hydrogen atoms alone, and from the Tully-Fisher relation,
ING BIENNIAL R EPORT 2004–2005 • 27 indicate that there must be far more matter in the Universe that can be accounted for by the visible light we see. This 'dark matter' still holds many mysteries for astronomers — is it well mixed up amongst the stars, or is it separate from the stars? Another puzzle is that the current ideas about how galaxies form predict that there should be many more galaxies in the Universe than are visible to us. So, these two ideas —dark matter and the lack of galaxies— have led to predict that there must be unseen 'dark' galaxies hidden in the Universe. Finding a dark matter galaxy is an important breakthrough because, according to cosmological models, dark matter is five times more abundant than the ordinary (baryonic) matter that makes up everything we can see and touch.
The members of the discovery team conclude that in the very nature of things it would be difficult to make an Figure 28. INT B-band optical image of the field of VIRGOHI 21. The cross marks the weighted center of the HI detection, and the indisputable claim to have found a dark galaxy, particularly circle shows the size and position of the central Arecibo beam. when past claims to that effect have quickly been ruled out by subsequent observations (either of a dim underlying galaxy or of bridging connections to nearby visible companions). Nevertheless, VIRGOHI 21 passed all of the careful tests the astronomers were able to set for it, using the best equipment currently available.
Dark galaxies are thought to form when the density of matter in a galaxy is too low to create the conditions for star formation. The observations of VIRGOHI 21 may have other explanations, but they are consistent with the hydrogen being in a flat disc of rotating material, which is what is seen in ordinary spiral galaxies.
MOST OF THE GROWTH OF SUPERMASSIVE BLACK HOLES IS Figure 29. The ellipse shows the region of sky where the dark OBSCURED BY DUST cloud was found on a colourful image from INT data. a galaxy with this velocity width would be expected to be Supermassive black holes underwent periods of 12 mag or brighter. exponential growth during which we see them as quasars in the distant Universe. Quasars are some of the brightest Deep optical CCD images in B, r', and i' bands with the objects in the Universe and are seen by the light emitted INT were obtained, reaching surface brightness limits of as gas and dust spiral into the black hole. They are 27.5, ~27.0 and 25.8 mag arcsec-2 respectively. On the B- situated in the inner-most regions of galaxies and can band frame, an object of 10" scale or larger at this surface consume the equivalent mass of between ten and a brightness limit should have been detected. This is more thousand stars in one year. It is believed that all quasars than 100 times dimmer than the central surface brightness are surrounded by a dusty ring which hides them from of the disks of typical spiral galaxies and dimmer than any sight on Earth in about half of cases. known massive low surface brightness galaxy or than the lowest surface brightness dwarf galaxy. The summed emission from these quasars generates the cosmic X-ray background, the spectrum of which has For many years astronomers have been measuring the way been used to argue that most black-hole growth is in which stars and galaxies move. These measurements obscured. There are clear examples of obscured black-
28 • ING BIENNIAL R EPORT 2004–2005 hole growth in the form of 'type 2' quasars, but their adding mass to the Galactic halo and provides an numbers are fewer than expected from modelling of the X- important probe of the shape of the dark matter potential, ray background. Objects surrounded by dust are hard to the lack of other major accretion events is somewhat see in visible light, so the astronomers looked at infrared disconcerting given the predictions from the ΛCDM. wavelengths. Using NASA's Spitzer Space Telescope data, they selected objects that have mid-infrared and The recently discovered Monoceros Ring (MRi, or the One radio emissions characteristic of quasars, but which are Ring) can be interpreted as an additional ongoing faint at near-infrared and optical wavelengths. accretion event within the Milky Way. Investigating the density and extent of this structure is important when The researchers found 21 examples of lost quasars in a trying to fully understand the impact this type of event is relatively small patch of sky. All of the objects were having on the evolution of our Galaxy both in the past and confirmed as quasars in radio wavelengths and using the into the future. If the MRi is instead the outermost edge of ISIS spectrograph on the WHT. This new population of the Milky Way, mapping the outer reaches of the disc will obscured quasars are hidden behind the dust of the provide insight into the past of the Milky Way. galaxy itself rather than just by a dust ring. The presence of lots of dust in a galaxy indicates that stars are still Astronomers used the INT Wide Field Camera to continue forming there. a campaign to detect this stellar population around the Galactic plane, mapping out the extent of the MRi in the Therefore, this population of distant type-2 quasars, which region of Galactic longitudes l =61°–150° with 10 pointings is at least comparable in size to the well-known in symmetric pairs above and below the plane of the unobscured type-1 population, is responsible for most of Galaxy spanning 90° about the equator of the Milky Way. the black-hole growth in the young Universe and, throughout cosmic history, black-hole growth has been This ongoing survey has yielded three detections of the concentrated in the dusty, gas-rich centres of active ring in the region l, b = (118°, 16°), (150°, 15°) and a galaxies. This is in good agreement with predictions from tentative detection at (150°, -15°). Galactocentric distance the X-ray background and implies, from comparisons estimates to these structures gave ~17, ~17 and ~ 13 kpc, between the integrated luminosity density of quasars (both respectively. These are combined with a re-examination of type-1 and type-2) and the local space density of relic the field observed with the INT WFC in 2003, (123°, -19°), black holes, that black-hole growth occurs in short, showing the position of the halo is not in accordance with efficient spurts in the cores of forming galaxies. the model and possibly represents another detection of the ring. The Galactocentric distance to this feature is estimated at ~21 kpc. This provides evidence that the ring THE INT/WFC SURVEY OF THE may be wrapped around the Galaxy more than once. MONOCEROS RING These detections also lie very close to the newly The formation and evolution of galaxies remains one of discovered structure in Triangulum-Andromedae hinting at the big questions in astronomy. In the currently favoured Λ a link between the two. The remaining six observed fields cold dark matter model (ΛCDM), galaxies are built up over are apparently non-detections although in light of the new time via accretion of smaller systems. One firm prediction models, closer inspection reveals tentative structure. of this model is that this accretion of smaller systems should still be ongoing and that the Milky Way halo should With the overdensity of M giant stars in Canis Major being contain a large number of satellite systems. It has been claimed both as a progenitor to the MRi and alternatively suggested that, given the model, there are too few a manifestation of the Milky Way warp, much is still satellites actually within the Milky Way halo. unknown concerning this structure and its connection to the MRi. The tidal dismemberment of a dwarf galaxy as it falls through the Milky Way halo is a slow process, with Both detections and non-detections support a complex extensive streams of tidal debris existing for long periods picture of the MRi. In particular, those detections above of time. While ancient remnants have been identified in our the plane suggest the MRi has an extended stream tracing own Galactic neighbourhood, more extensive surveys of an arc ~17 kpc from the Galactic Centre, while the the Galactic halo have concluded that there is only a detections below the plane, reveal a tentative detection of single, major ongoing accretion event, that of the the Triangulum-Andromedae region in the background of Sagittarius dwarf galaxy. While this accretion event is the (123°, -19°) region and also the presence of a
ING BIENNIAL R EPORT 2004–2005 • 29 foreground stream. Lying roughly in the plane of the Milky or alternatively, the MRi may be a natural part of the disc Way, the MRi may represent a unique equatorial accretion formation process. event which is contributing to the thick disc of the Galaxy,
Figure 30. Aitoff projection of the sky, illustrating the locations of the fields obtained for this current survey. The projection is in equatorial coordinates, with the Milky Way equator (b= 0°) shown as a solid black curve accompanied by the dashed curves which mark out Galactic latitudes of b=±20°. The Galactic Centre (l= 0°) and anticentre (l= 180°) are shown as solid bars crossing the Galactic equator. The points represent the prograde model for the destruction of the Canis Major dwarf with the grey-scale showing the Galactocentric distance (kpc) of the points, as shown in the side bar. The dense knot located below the Galactic equator represents the final location of the progenitor used in the simulation. The symbols in the plot are represented as follows: the circles represent the location of the fields in this survey; the squares represent the fields associated with the M31 survey, with the hashed squares being confirmed detections of the ring and empty squares being non-detections.
30 • ING BIENNIAL R EPORT 2004–2005 Chapter 2
OPERATION, MAINTENANCE AND DEVELOPMENTS
TELESCOPE OPERATION Adaptive optics observations are gradually becoming more important. The advent of the laser guide star system During the two-year period 2004/05 covered by this report, in the near future will drastically enhance the scientific the ING telescopes again performed very well, with potential and hence likely increase the interest in the use downtime figures due to technical problems averaging of adaptive optics further. In order to ensure optimal only 2.3% and 1.5%, on the William Herschel Telescope scientific use of the best seeing periods for adaptive optics (WHT) and the Isaac Newton Telescope (INT), observations the observing programme at night must be of respectively. These figures are well below the target value a flexible nature. The expectation is that during certain of a maximum of 5 percent technical downtime. Observing periods of the year the WHT will be operated in such time lost due to poor weather over the same period queue-scheduled mode. averaged 34%. The presence of the Isaac Newton Group of Telescopes at Day-to-day telescope operations support is carried out by the Spanish Observatorio de Roque de los Muchachos a dedicated Operations Team, taking responsibility for the (ORM) is secured under international agreements. These telescopes and associated infrastructure. Efforts of day- agreements will be up for renewal around the turn of the time and night-time support activities concentrate on the decade after having been in force for 30 years. Leading up WHT. On this telescope five common-user instruments are to this date discussions between the various international supported, one of which is the complex adaptive optics partners are under way on how best to adapt and continue suite. Also several visiting instruments were supported at with the formal structure in order to prepare the wider the WHT. Many observing teams visit the telescopes every observatory for the future. In parallel with these year. The INT, in contrast, operates in a much simpler discussions, ideas have further matured on potential fashion and is a single-instrument facility. The 1-m JKT further collaboration between telescope groups at the does not host science observations anymore, but is now observatory, building on the successful collaboration that regularly being used for measuring the atmospheric already exists with the Italian 3.5-m Telescopio Nazionale turbulence profile above the observatory using the Galileo (TNG). technique of SCIntillation Detection And Ranging Together with the international agreements also the (SCIDAR) led by the IAC. telescope facilities advance in age. One of the first telescopes at the ORM was the INT. In February 2004 that At night a telescope operator in always present on the telescope had been in operation on La Palma for 20 years. WHT to assist the scientists in taking the observations. An impressive period of two decades of continuous ING’s team of astronomers acts as the primary contact for operation that has resulted in many important discoveries visiting scientists. They assist visitors in taking the and well over 1100 papers published in scientific journals. observations and in carrying out observations in service for the community. INSTRUMENTATION The year 2005 marked the end of an important reorganisation that was the result of a phased reduction of An important development for the WHT was the operating cost of the observatory. These measures commissioning and first science operation of the unavoidably had an impact on the service delivered to the intermediate resolution IR spectrograph and imager, visiting astronomers, but the strong focus on the operation LIRIS, that was built by the Instituto de Astrofísica de of the WHT has meant that a continued high level of Canarias. This instrument, based on a 1024 by 1024 pixel service and flexibility could still be offered to the Hawaii array detector operates in the Cassegrain focus of community of users. the telescope and allows high quality imaging and multi-
ING BIENNIAL R EPORT 2004–2005 • 31 Figure 32. I-band image of a close binary star with the NAOMI Figure 31. LIRIS mounted in the Cassegrain focus of the WHT. Adaptive Optics system using the OASIS integral field spectrograph. object spectroscopy at near IR wavelengths. Following extensive testing LIRIS was taken into operation during the summer of 2004 as a common-user instrument. The science projects carried out with this instrument are diverse and include distant galaxies, stellar populations, brown dwarfs and planetary nebulae, showing the potential of this instrument for the community of users. In particular the possibility of using multi-object masks offers a potential that is currently a rare feature at other telescopes.
Since its commissioning LIRIS has become one of the most popular instruments on the WHT. Its multi-slit mask mode is particularly popular as it offers a huge multiplex advantage over classical long-slit spectroscopy and is therefore very efficient. Many spectra of for instance galaxies in distant clusters can be observed at the same Figure 33. The automatic dichroic filter changer unit. time. Also during the year the polarisation module was commissioned in LIRIS, offering imaging polarimetry at modes. Also optical imaging can be conducted with this infrared wavelengths. system, and best images achieved so far have been those of a close binary system, achieving 0.1 arcsecond image Development work at the ING has focussed on the width in the I band. Adaptive Optics (AO) instrumentation suite, an extensive and rather complex set of instruments that permanently The OASIS spectrograph supports a wide choice in occupies one of the Nasmyth foci at the WHT. The bandwidth and resolution. OASIS competes for photons Adaptive Optics system itself, NAOMI, has been in with the wavefront sensor, and in order to have the best operation for four years now. It feeds three science possible throughput to both OASIS and the wavefront instruments: the infra-red imager INGRID, the sensor a range of dichroic beam splitters is available to coronagraph OSCA, and the optical integral field pre-select the wavelength range of interest. The dichroic spectrograph OASIS. The latter is the most recent addition reflects the appropriate waveband into OASIS while the to the AO capability through a collaboration with the remaining photons are used for wavefront sensing. Until Observatoire de Lyon, France. recently manually changing dichroic filters posed a significant operational overhead, and therefore an The OASIS adaptive-optics assisted integral field automated system was designed and built to swap spectrograph was taken fully into operation during the dichroics in and out of the beam in a fast, accurate, and reporting period. The spectrograph works in the optical efficient manner. This dichroic changer was commissioned wavelength range and offers a wide variety of spectral during the reporting period and is currently in full operation.
32 • ING BIENNIAL R EPORT 2004–2005 infrared wavelengths from a few percent to nearly 100%. In terms of astronomical research, this translates into radical progress as it opens up high spatial resolution observations from the ground to nearly all types of science targets, making possible the observations of faint and extended sources, and enabling observations of large samples, unbiased by the fortuitous presence of nearby bright stars. In combination with the existing instrumentation the WHT will offer a highly competitive facility to the astronomical community, exploiting a window of opportunity before similar capability will exist on 8-m class telescopes. Figure 34. The Low-Light-Level CCD that will be deployed as wavefront sensor in the AO system. The actual CCD chip is the The system design of GLAS was fully completed in 2005. tiny black square in the yellow enclosure. At the heart of the system will be a 515nm green laser of about 30W. This laser will be mounted at the top of the Natural guide star adaptive optics is largely limited by the telescope. Its light beam will travel to the centre of the availability of stars bright enough to measure the telescope, behind the secondary mirror, where it will be wavefront distortions on that are induced by the Earth’s injected into a beam launch telescope. There the laser atmosphere. Measurement and correction of the beam will be expanded to about 35cm, and subsequently wavefront distortions has to take place in the shortest projected into the atmosphere where it will be focussed at possible time in order to generate the best results. a distance of 20km. The diagram below gives a good However, short exposure times (milliseconds) also imply impression of what this part of the system will look like that few photons are available and hence bright stars are once installed at the WHT. Expectation is that the laser required to generate sufficient signal-to-noise. Also in the system will be commissioned in 2006. case of NAOMI this is a limitation for effective and broad scientific use of the instrumentation. Being able to detect Existing instruments remain competitive through the fainter stars would help ease the situation. At very faint continuous upgrade and improvement of its components. signals the detector read noise becomes an important Therefore, apart from the major new instrument factor, and therefore a project is under way to install a developments mentioned above, there have also been a zero-read noise CCD in the existing wavefront sensor. For wide range of enhancements to instruments, all with the faint guide stars the nearly zero read noise from this new aim to improve the scientific capability and operational detector is expected to improve the detection efficiency of the system by at least a factor of two.
The ultimate solution for finding bright enough guide stars is to create an artificial ‘star’ that can be used as a wavefront sensor source. Such artificial source can be created using a strong, well collimated laser beam that is aligned with the main telescopes. Laser light that is back scattered from high in the atmosphere can then be used as an artificial point source suitable for wavefront sensing. In 2004 a project was initiated to create such laser beacon based on Rayleigh back scatter from an altitude of about 20km above the observatory. This project, listening to the Dutch acronym GLAS, for (translated) Ground-layer Laser Adaptive optics System, will work in conjunction with the NAOMI instrument as well as with the existing science cameras. Figure 35. Top ring of the WHT, with shown in the front the laser unit inside a cradle. Laser light will travel through an evacuated The scientific advantages of GLAS are potentially huge as pipe to the centre of the telescope, where it will be projected into such a laser guide star system will amplify the fraction of the atmosphere by the beam launch telescope that is located sky available to adaptive optics observations at visible and behind the secondary mirror.
ING BIENNIAL R EPORT 2004–2005 • 33 sharper cut between the wavelength ranges at a wavelength that is appropriate for most science programmes, and also features a smoother response. A small but very significant upgrade that has helped the efficiency of the instrument as a whole.
The WHT remains very popular with university groups who build dedicated instruments to find answers to specific astronomical questions. The infrastructure and support offered by ING greatly assists the exploitation of visiting instruments. For that reason over the years many instruments have been deployed in this way and during the reporting year no less than six different visiting instruments came to the telescope. New instruments that Figure 36. WYFFOS long camera. had not been to the WHT before were the CIRPASS multi- object IR spectrograph and PLANETPOL, capable of extremely high accuracy polarimetric observations. A brief description of these two new visiting instruments follows.
CIRPASS is a near-IR fibre-fed cooled spectrograph, designed and built by a team from the University of Cambridge. The acronym stands for the Cambridge Infra- Red Panoramic Survey Spectrograph. CIRPASS can take either an integral field fibre bundle or a multi-object fibre bundle. The latter was used at the WHT. A plug-plate system of pre-drilled holes allowed the acquisition and observation of many galaxies simultaneously, thus
Figure 37. Response curve of the new dichroic of the ISIS providing a huge multiplex advantage. The observations spectrograph. focussed on the star formation rates in distance galaxies such as those found in the Hubble Deep Field. efficiency. An important milestone was achieved with the The second visiting instrument new to the WHT was successful commissioning of the WYFFOS long-camera. PLANETPOL, from the University of Hertfordshire (UK). This new camera to the fibre-fed WYFFOS spectrograph The key objective of this instrument is to detect and has the advantages over the original camera that it characterise scattered light from planets around distant accommodates a larger number of fibres, has an external stars. Starlight scattered on the surface and in the focus permitting change of detector, and provides a atmospheres of extra-solar planets causes a weak but somewhat higher spectral resolution than the previous camera. The camera was built by the ASTRON institute in characteristic polarization signal. PLANETPOL is the Netherlands. designed to detect such very weak signals and has already proven it can achieve that demanding goal. Apart from the hardware changes for the WYFFOS instruments, there have also been very significant The WHT also keeps attracting experimental activities. upgrades of the software. In particular the software Arguably the most exciting set of experiments relate to the responsible for setting up the multiple fibre module, future development of extremely large telescopes. The AUTOFIB, that feeds WYFFOS has seen major future telescopes will have segmented primary mirrors modernization, resulting, amongst other things, in a and a very significant and costly problem is the control of drastic reduction of the fibre setup time. the segments in order to keep them aligned at all times to a fraction of a wavelength. Of course this problem has Also the venerable ISIS spectrograph has seen important been solved by existing segmented telescopes such as advances with the acquisition of a new dichroic filter that the Keck twins on Hawaii and the GTC on La Palma, but splits light between the red and blue optimized for future ELTs the problem is much more severe and spectrograph arms. The new dichroic possesses a costly. Therefore alternative methods are being
34 • ING BIENNIAL R EPORT 2004–2005 Figure 38. The CIRPASS IR spectrograph (blue cabinet) being positioned on the moving platform at the base of the WHT. Light Figure 39. The PLANETPOL instrument mounted in the from the Cassegrain focus is fed through a large bundle of fibres Cassegrain focus of the WHT, together with the team of scientists. to the spectrograph. considered to determine the phase difference between the segments by optical means, in a fast way, and by using starlight. The results of such measurement can then be used to mechanically control the relative position of the mirror segments.
Theoretical work by the group in Arcetri, Italy showed the feasibility using a novel technique of the pyramid wavefront sensor, but this required testing under real conditions as proof-of-concept. This idea inspired Figure 40. Picture of WHT telescope pupil as see through the collaboration with groups from Durham, UK to use the pyramid wavefront sensor. The resulting mirror flatness over the deformable mirror of the NAOMI adaptive optics system controlled subset of mirror elements was better than 10nm. which happens to have individual segments that can be controlled, thus serving as a tiny prototype of a future giant telescope. The experiments were very successful and have proven that the concept is indeed viable.
Another very successful experimental activity that was hosted by the ING falls in the field of astronomical site characterization. In past years researchers from the University of Durham had developed a novel method to measure atmospheric turbulence. This method of Slope Detection and Ranging, or SLODAR, had been extensively tested on the WHT and was so successful in measuring turbulence profiles in the lower atmosphere that a portable unit was designed. This unit would be deployed at different observatories as a site testing tool in Figure 41. First deployment of the SLODAR equipment. preparation for the future construction of extremely large telescopes. First tests were carried out on La Palma, 'parking' area was constructed in the basement of the hosted by the ING. WHT. In this enclosure the instrument can be kept cold and connected to the network and ancillary equipment for INFRASTRUCTURE monitoring and control. Furthermore, a mobile, deployable clean room has been acquired that can be installed in the The LIRIS IR spectrograph was commissioned during the aluminizing area. The prime purpose of this acquisition reporting period. LIRIS, being a complex cryogenic was for LIRIS in case the instrument needs to be opened instrument, requires particular care also when it is not up, but it will be equally useful for similar operations on mounted on the telescope. For that reason a dedicated other instruments.
ING BIENNIAL R EPORT 2004–2005 • 35 An important milestone was reached with the full modernization of the detector controller infrastructure. Not only the science detectors, but also all TV and autoguider systems now operate on the basis on SDSU controllers while data acquisition runs through ING's ULTRADAS software system. Having a uniform infrastructure for these systems offers significant advantages for maintenance, while at the same time performance of these modern systems is much better.
Steady progress was made on installation of a higher bandwidth data link between the Mayantigo office building Figure 42. Lifting of primary mirror of the Nordic Optical Telescope at sea level and the observatory site, culminating in an in preparation for aluminizing. order-of-magnitude enhancement. Also the connection of the observatory to the Internet improved drastically. This During the reporting period both the INT and WHT primary improvement has meant, amongst other things, that mirrors were re-aluminized. Also mirrors from partner archiving of scientific data in Cambridge is now automated telescopes at the observatory make use of ING’s and does not require posting of tapes or disks anymore. experience and infrastructure. The past two years both the mirror of the Nordic Optical Telescope and of the Liverpool Over the years ING has been making steady progress in Telescope were aluminized by ING. tracking and implementing the latest CCD detector technologies. Activities include the use of low-light-level Early in the reporting period the SUPERWASP CCDs for wavefront sensing as well as for high speed experiment, led by the Queen’s University Belfast and spectroscopy, optimized coatings to reduce fringing at hosted by the ING was officially inaugurated. The long wavelengths, and testing of surface treatment installation consists of a number of wide-field cameras on techniques also to reduce fringing. a robotic mount, located in an automatic roll-off roof enclosure. The main scientific aim of this experiment is the A low-key activity has been the step-wise improvement to detection of planets around stars through their occulting the WHT control room, in order to make it a more friendly effect when the planet transits the stellar surface. The work environment, including new furniture, additional inauguration event was carried out, very appropriately, by possibilities for computer connections, and improvements remote control; the mayor of the municipality of Garafía in lighting, computer screens and insulation from the where the observatory is located, Mr. José Peñate, somewhat noisy electronics cabinets. commanded the instrument to move and cut a red ribbon.
Figure 43. Left: SuperWASP inauguration by remote control. Right: Enclosure open of SuperWASP and WHT dome in the background.
36 • ING BIENNIAL R EPORT 2004–2005 Chapter 3
USE OF OBSERVING TIME AND SCIENTIFIC PRODUCTIVITY
USE OF TELESCOPE TIME Stand-down and discretionary nights are used for major maintenance activities, commissioning of new The available observing time on the ING telescopes is instruments, enhancements, calibration and quality control allocated between British, Dutch and Spanish time tests, etc., and partly for astronomy, for example, as allocation committees, the CCI International Time compensation for breakdowns or for observations of Programmes (ITP), service and discretionary nights, and targets of opportunity. scheduled stand-down and commissioning time. The way the available observing time on the ING The ING Board has delegated the task of time allocation telescopes has been shared in 2004 and 2005 is to British astronomers to the PPARC Panel for the summarised in Table 1. Allocation of Telescope Time (PATT), and to Dutch astronomers to the NFRA Programme Committee (PC). It USE OF INSTRUMENTATION is the responsibility of the Instituto de Astrofísica de Canarias (IAC) to allocate the Spanish time via the Comité Figure 44 shows the allocation of nights per instrument on para la Asignación de Tiempos (CAT). For committee the WHT in 2004 and 2005. As in previous years, the ISIS membership see Appendix I. spectrograph was the most popular instrument, taking up some 40% of the scheduled observing time. Visiting The aim of the ING service observing programme is to instruments on the WHT during this period include the provide astronomers with a way to obtain small sets of SAURON integral field spectrograph, the planetary nebula observations, which would not justify a whole night or spectrograph, PN.S, the high-speed multi-CCD camera more of telescope time. On the WHT several nights per ULTRACAM, the near-IR multi-object spectrograph, semester are set-aside especially for this purpose. During CIRPASS, and the PLANETPOL photo-polarimeter. The those nights, ING support astronomers perform INTEGRAL coherent fibre feed to the WYFFOS observations for several service requests. spectrograph is effectively operated as a private
WHT INT Time allocation 2004 2005 2004 2005
UK PATT 139 130 174 163 NL PC 49 56 61 63 SP CAT 77 78 104 100 ITP 8 14 8 14 TNG time share 10 11 — — Service 19.5 17 — — Instrument Builder’s Guaranteed Time 17 19 0 0 Stand-down and discretionary 46.5 40 19 25 (including commissioning)
Total 366 365 366 365
Table 1. Number of nights allocated from Semester 2004A to 2005B. Service include UK and NL service time, and SP CAT includes Spanish service time.
ING BIENNIAL R EPORT 2004–2005 • 37 Figure 44. Use of WHT’s instrumentation per semester. Figure 46. Weather downtime per year. instrument as well. In particular the ULTRACAM and PLANETPOL instruments enjoyed much interest.
On the INT, dark time periods were exclusively used for CCD imaging with the Wide Field Camera, as the INT was solely dedicated to wide field imaging programmes.
TELESCOPE RELIABILITY
During the year 2004 and 2005 the ING telescopes again performed very well, with downtime figures due to technical problems averaging at 3.4% and 1.5% in 2004 and 1.5% and 1.4% in 2005 for the WHT and the INT respectively. These figures meet the target value of a maximum of 5% technical downtime. Down time due to poor weather averaged 35% in 2004 and 34% in 2005. The historical trends of technical down time and weather down time are plotted in Figures 45 and 46. Figure 47 shows the seasonal average. Figure 47. WHT’s monthly weather downtime.
SCIENTIFIC PRODUCTIVITY Appendix E) is updated annually. Traditionally, this bibliography has been compiled by visually scanning all An important metric of the success of the ING telescopes articles in many journals and identifying those which make is the number of publications published in refereed use of data from our telescopes. However most journals journals and for this reason the ING Bibliography (see are now published electronically and often have quite sophisticated search engines associated with them and it is therefore appropriate to conduct the search with the help of these facilities.
Our selection process identifies papers that make direct use of observations obtained with the ING telescopes, in order to qualify. Papers that refer to data presented in earlier papers (derivative papers) are not counted.
When we analyse ING publications for the five years between 1995 and 1999 inclusive it can be seen that more than 95% of articles are published in a small number of Figure 45. Technical downtime per semester. core journals. These core journals consist of the British
38 • ING BIENNIAL R EPORT 2004–2005 journal MNRAS, the American journals Astrophys J, Astrophys J Letters, Astrophys J Suppl, Astron J and PASP, plus the European journal Astron Astrophys (including the now defunct A&AS). We also include Nature and Science as core journals due to their perceived high impact. Journals making up the remainder of publications are widely spread among such journals as Icarus and the Irish Astronomical Journal to name a few. The bibliography for the years 2004 and 2005 was compiled from only the core journals listed above for reasons of efficiency. Search engines were used to select papers and the resulting list of papers visually inspected to ensure that they satisfied the selection criteria described above. Figure 48. Number of refereed papers per telescope from first light year.
An analysis of these numbers follows (see Figures 48 to 52 and Table 2). Note that if a paper makes use of more than one telescope we count that paper for each telescope. Also, concerning perceived nationality we use the nationality of the first author's institution although in a few cases two institutions are credited. Similarly, if a paper makes use of more than one instrument, that paper is counted against each instrument.
Of all the available instruments on the WHT, the ISIS spectrograph remains the most productive instrument, with 42% of all publications during the reporting period. The number of papers from visitor instruments on the WHT also remained significant, with 16 papers over two years.
On the INT the papers are split very evenly between IDS spectrograph and the Wide Field Camera as might be Figure 49. Accumulative number of refereed papers per year. expected from the split of observing time between these instruments, roughly 50-50. Year WHT INT JKT Total 1984 — 1 — 1 Concerning the nationality of the first author's institution, 1985 — 10 3 13 there is little change, at least considering the fluctuations 1986 — 24 8 32 1987 — 36 16 52 from year to year. The UK share is steady around 40%, 1988 5 52 12 69 and the Spanish share about 20%. The NL share also 1989 15 58 15 88 showed little systematic change. Interestingly, about one 1990 37 54 26 117 1991 39 63 19 121 third of the papers have a first author from other countries, 1992 42 56 25 123 emphasizing the international character of the observatory 1993 55 70 30 155 1994 78 63 44 185 and the high level of international collaboration between 1995 90 81 29 200 research groups. 1996 100 84 52 236 1997 113 77 35 225 1998 118 72 38 228 THE ING ARCHIVE 1999 115 78 46 239 2000 78 53 31 162 2001 91 46 25 162 All data taken with the ING telescopes is archived in the 2002 93 72 26 191 UK, at the Institute of Astronomy, Cambridge. The data 2003 82 44 17 143 2004 103 69 26 198 archive is managed by the Cambridge Astronomy Survey Unit. 2005 77 80 18 175
Archival data from the ING telescopes is made available to Total 1333 1243 541 2743 anyone upon request, after a one-year proprietary period. Table 2. Number of refereed papers per year and telescope.
ING BIENNIAL R EPORT 2004–2005 • 39 Figure 50. Top: Use of instrument data in WHT refeered papers in Figure 51. Top: Use of instrument data in INT refeered papers in 2004. Archival papers made use of data from ISIS, PFIP, UES, 2004. Archival papers made use of data from the PFIP, WFC and INGRID and AUX. Bottom: The same in 2005. A total of 12 papers IDS. Bottom: The same in 2005. A total of 6 papers resulted from resulted from data obtained on service nights in both years. data obtained on service nights in both years.
Figure 52. Evolution of the nationality of first author’s first institution in ING refeered papers. Figure 53. Number of ING archive requests per year.
The number of archive retrieval requests has remained high over the past two years, with over 500 requests per year, for retrieval of more than 40,000 data sets. The historic trend of the archive requests can be seen in Figure 53. This level of archive use underlines the importance of the ING archive as a general tool for astronomy research.
40 • ING BIENNIAL R EPORT 2004–2005 Chapter 4
IN-HOUSE RESEARCH
The in-house research effort at ING comprises 1 full-time equivalent (FTE) from its recurrent operational budget, an additional 2 FTEs contributed by PPARC. This effort is distributed amongst 9 members of the Astronomy Group which includes the Head of Astronomy, 6 support astronomers and 2 PPARC research fellows. In addition to these staff there is an additional research astronomer (Dr. Evans) funded through a PPARC Postdoctoral research grant award to Dr. Lennon.
During the years 2004 and 2005, ING staff's research productivity, as measured by publication rate was maintained at its previous high level, publishing approximately 200 papers in various scientific publications, approximately 50% of these appearing in refereed journals. A complete list of these papers is included in Appendix F. As in previous years, an important aspect of the research effort is that ING staff continue to be closely involved with on-going research programmes which are heavily dependent on observations carried out on our telescopes. An important example of this synergy is ING’s very active role in the INT/WFC Hα survey of the north Galactic plane (the IPHAS survey, PI: Prof. Drew), which involves 6 ING staff (Corradi, Greimel, Lennon, Leisy, Figure 54. IC1396, the Elephant Trunk Nebula, is a giant cloud of Skillen and Evans) and makes use of their expertise with gas and dust is illuminated by a massive central star whose radiation is triggering star formation throughout the region. This the Wide Field Camera, for the survey, and with AF2, for image was obtained as part of the IPHAS survey. Field of view is the spectroscopic follow-up. An excellent example of approximately 15×20 arcmin, North to the left, East is down. collaboration with other facilities on the Roque de Los Muchachos Observatory is typified by Ian Skillen’s detached BAL trough, and the second-largest radio involvement with the SuperWASP facility, this project rotation measure known. This suggests that the quasar is kicked off in 2004 and aims to carry out an ultra-wide-angle intrinsically unusual (probably due to an exceptionally high survey of the northern sky. In addition Licandro co- accretion rate and also a high Eddington ratio), rather than ordinated a multi-telescope monitoring campaign focused merely viewed at an unusual angle, as has often been on Deep Impact, more of these and other activites are posited to explain the peculiar properties of BAL quasars. discussed below. This work was carried out in collaboration with Carballo and González (Santander), Holt (Sheffield), Vigotti and INDIVIDUAL RESEARCH ACTIVITIES Mack (Bologna), and Perley (NRAO). He also co- supervised (with Ellison, Victoria, Canada) an investigation Benn investigated the properties of the most radio- by Russell (1-year student at ING) into quasar damped-Ly- luminous broad-absorption-line (BAL) quasar known α absorbers (DLAs), finding that there is an excess at low (1624+3758), discovered during his earlier INT search for velocities (v<6000 km s –1) relative to the quasars, i.e. the high-redshift radio quasars. The quasar is highly unusual, properties of the DLAs can be used to constrain clustering with prominent FeII UV191 1787-A emission, a broad near high-redshift quasars.
ING BIENNIAL R EPORT 2004–2005 • 41 In collaboration with Furness (1-year ING student), Schirmer (ING) and Sánchez (Calar Alto), Benn obtained a sample of z~4.5 Ly-α galaxies from a deep imaging search at the INT. This is the first stage of a search for the expected dramatic decline in galaxy counts marking the epoch of re-ionisation.
Sánchez and Benn published an analysis of astronomical productivity by country (a follow-up to their earlier analysis of the scientific productivities of telescopes worldwide).
Corradi studied several aspects concerning Galactic and extragalactic planetary nebulae (PNe). A significant result was the detection of systems of concentric rings around Figure 55. The newly discovered Planetary Nebula PN the main bodies of the nebulae (previously known only in 126.62+1.32, the ‘Prince of Asturias’, is a rare quadrupolar nebula few PNe) around a large fraction of the PNe that were and it was discovered using IPHAS data. properly imaged. This implies that the mass loss modulation producing the rings in the last 10,000–20,000 data were used to present a comprehensive atlas of ultra- years of the AGB evolution must be a rather ubiquitous violet spectra of metal-poor massive stars. The use of this phenomenon, and therefore should be included in any atlas for synthesizing the UV spectra of high-redshift star physical model describing the critical mass loss that takes forming galaxies was also a highlight of this project (in place in this phase. collaboration with Rix), as was its use to investigate the nature of the super star clusters in NGC1705-1. A thourough study of the dynamics of the multi-polar nebula Mz3 was performed, showing an enigmatic system Trundle & Lennon published a comprehensive study of B- of 4 distinct outflows with different degrees of collimation. type supergiants in the Small Magellanic Cloud, At present, none of the existing theories can explain such uncovering a serious discrepancy between observed and a complex mass loss behaviour from an evolved star. theoretical mass-loss rates with important implications for our understanding of mass-loss in luminous blue variables, Concerning extragalactic PNe, their search using the and the physics of mass-loss in these kinds of stars. They observation from the Local Group Census survey was nearly also also found very high surface nitrogen abundances in completed, and follow-up spectroscopy with the aim of these stars, typical enhancements being an order of determining their chemical properties was presented for the magnitude higher than the pristine SMC nitrogen abundance. nearby spiral galaxy M33. This extends our knowledge of the galaxy’s chemical content at intermediate ages of its evolution. Evans published the first results of a 2dF survey of massive stars in the Small Magellanic Cloud, this seminal Greimel has worked with Augusteijn (NOT) on the paper providing a rich dataset comprising 4161 spectra, selection of red dwarf-white dwarf binaries from the SDSS. mostly of B and A giants/supergiants. He has also He is also involved in the Hα survey of the Milky Way published several core papers on detailed analyses of (IPHAS) and its follow up observations. Together with massive OB stars in the Magellanic Clouds which were Corradi (ING), Viironen and Mampaso (both IAC) he instrumental in revising their effective temperature scale. participated in the compact PN search; together with Lennon & Evans also spent considerable time working on Steeghs (CfA), Drew and Unruh (both ICL) he defined the the ‘VLT-FLAMES Survey of Massive Stars’, a Large VLT Hectospec and AF2 follow up observations. He also project which will ultimately produce, as part of its brief, defined the IPHAS variable star candidate list of which detailed analyses of approximately 1000 OB stars in the follow up observations have started in collaboration with Galaxy and the Magellanic Clouds. Evans is the lead Robb (Victoria, Canada). author on the first two consortium papers submitted to A&A, while there are several other papers in preparation or Lennon, together with Evans (postdoc) and Trundle (PhD already submitted. student) completed the most definitive study to date of massive star wind terminal velocities in the Small Evans and Lennon also continued their involvment in large Magellanic Cloud. This work was based on extensive scale spectroscopic surveys with contributions to the allocations of HST/STIS observing time, and the same IPHAS follow-up spectroscopy, completing the preliminary
42 • ING BIENNIAL R EPORT 2004–2005 classification of several thousand spectra in selected help to better constrain what happened during the first IPHAS fields (with student intern Mansura Jaigirdar), and stages of the formation of the first galaxies. contributed to the formulation of a large programme aimed at surveying the Magellanic Clouds. Licandro carried out a spectral (visible and near-infrared) survey of trans-neptunian objects (TNOs) and related icy Rix has published a pioneering paper that promotes the minor planets, and also studied the physics of cometary use of new metallicity indicators, based on iron absorption comae. He was also the P.I. of the international campaign features, for measuring the chemical enrichment of high at the ORM in support of the Deep Impact mission. Comet redshift star-forming galaxies. This work was based mainly 9P/Tempel 1 was observed for several months before the on theoretical synthetic spectra, and she has now turned impact with the TNG, and during 10 days around the her attention to applying them to observed spectra. Rix has impact, from July 2 to July 10, was observed also pursued her work on quasar absorption line systems. simultaneously with the WHT, TNG and NOT telescopes. In 2004 she was the co-author on a paper that quantified Images in the visible and near-IR low and high resolution the possible impact of dust from intervening galaxies on spectra in the visible and near-IR, were obtained. The data, QSO absorber statistics.She is now collaborating with still under analysis, offer a unique opportunity to study the Pettini (IoA) in a project to study the detailed physical and properties of the dust ejected by the impactor (amount of chemical properties of a proximate damped Ly-α absorber. dust ejected, size distribution, etc), and to study also the gas produced after the impact. In her role as ‘XOasis support’ for the ING’s OASIS instrument, Rix is also involved in a research project with The visible and near-IR spectra of several TNOs, Centaurs Lennon and Parker (1-year ING student) to study the and comet nuclei were obtained during 2004-2005. circumstellar properties of the Luminous Blue Variable Particularly important is the discovery that the surface of (LBV) P Cygni. This project exploits adaptive-optics 3D TNO 2005 FY9, the third largest known TNO, is very spectroscopic observations from the WHT’s OASIS similar to that of Pluto. The spectrum is dominated by the +NAOMI instrumentation suite. strong methane-ice absorption bands. The observed bands are deeper than those in Pluto's spectrum, which is Leisy continued his study of extragalactic planetary indicative of a larger fraction of methane-ice and/or nebulae (PNe). He published two articles about new PNe methane-ice with larger particle size in the surface of this candidates in Local Group (LG) Galaxies and one about bright TNO. This study reveals that 2005 FY9 is an the abundance determinations of 180 PNe in the LMC and excellent candidate to be the second. known TNO with a SMC. A search for fainter PNe, hopefully also very metal bound atmosphere (Pluto is until now the only case of a poor, has been started in the SMC and the bar of LMC, as TNO with atmosphere). well as in other Local Group galaxies with the Local Group Census survey (with the WFC and the ESO 2.2m WFI). Other important results are those revealed by the study of the spectrum of TNOs Quaoar and 2002 TX300, using Many new candidates have been found in several galaxies, and most of them are already spectroscopically confirmed. The main goal is to produce catalogs of emission line objects, and then to do spectroscopic follow- up, mainly of PNe and HII regions. The main goals are to determine abundances and to confirm membership of some of the candidates lying very far away from their parent galaxy centers (with high resolution spectroscopy at the WHT/AF2 for example). Four Local Group galaxies (Sextans A and B, IC1613 and NGC3109) have also been observed with the VLT/FORS2 and and time was awarded on Gemini North to observe some additional northern galaxies.
These spectra are used to derive chemical abundances, Figure 56. J-band image of comet Tempel 1 obtained using LIRIS on the WHT on July 4th, 2005. The image is the division of July both to better understand the stellar evolution of 4th by July 3rd images. A clear jet structure is visible in South- intermediate mass stars and the chemical evolution of West direction (on the image, North is up, East is left). The field of galaxies in the Local Group and beyond. The very view of the image is 50×50 arseconds on sky which corresponds important effects of nuclear processes at low metallicity will to about 32,000 kilometres at the distance of the comet.
ING BIENNIAL R EPORT 2004–2005 • 43 scattering models. Both large TNOs present interesting databank that has now been released for public use. surface properties. Quaoar presents a large fraction of Østensen also organized the 2nd Meeting of Hot Subwarf cristaline water-ice on the surface, and clear indications of Stars on La Palma during 2005. other volatiles, probably methane-ice. 2002 TX300 present the strongest ever observed water ice absorption Schirmer continued his work on the selection of galaxy bands, it spectrum is similar to that of Charon. This is the clusters using weak gravitational lensing techniques. Such first Charon-like TNO observed. The spectra of all these a mass-selected sample of galaxy clusters is of great large TNOs reveal that their study is very important to cosmological interest, since clusters of galaxies indicate understand the resurfacing processes that make that large the highest dark matter density peaks in the Universe, and TNOs exhibit fresh volatiles in their surface. therefore retain a memory of the initial conditions for structure formation. From a 20 square degree survey 30 Méndez and colleagues completed the search for the candidate galaxy clusters have been selected, and Mischa companion star to Tycho SN 1572, which followed the applied for multi-object spectroscopy time for further publication of a paper in Nature (P. Ruiz-Lapuente et al., detailedinvestigation. If confirmed, these clusters will form 2004, Nature, 431, 1069). The research team found a the currently largest sample of mass-selected dark matter subgiant star, named as 'Tycho G', whose proper motion haloes. The main collaborators in this project are Matturi was too high for its Galactic location and in the range of (Padova), van Waerbeke (UBC Vancouver) and the expected gained momentum at the supernova time. Schneider (Bonn). The same survey data forms the basis This and other features led the discovery team to conclude of several other projects Mischa is involved in, such as that Tycho G was the companion star to Tycho SN at the studies of the dark matter haloes of galaxies (Kleinheinrich time of the explosion. Méndez also continued to et al.), populations of Lyman-break galaxies at various participate in observations for and preparation of papers redshifts (Hillebrandt et al.), the galaxy dark matter bias by the Supernova Cosmology Project, the Physics of Type (Simon et al.) (all University of Bonn), or a census of tidal Ia Supernova Explosions (RTN) and the European tails (Pohlen et al., IAC). Supernova Consortium (ESC) collaborations. He also researched the history of the ING, and participated in the Within the framework of ING, Leisy and Schirmer are organisation of several international conferences and in searching for planetary nebulae in Local Group galaxies public outreach activities. and beyond, significantly improving their detection efficiency by means of sophisticated data reduction Østensen is continuing his work with the ING Adaptive schemes. Together with Chris and Furness he participates Optics group, where his work has focused on in the search for Lyman-break galaxies at redshifts of 4 characterisation of AO performance. In his research he and beyond. Other of his projects encompass the has continued his ongoing work on pulsations in subdwarf identification of unknown gamma-ray sources in the B-type stars, discovering a number of new pulsators as Galaxy (La Palombara et al., Milan), X-ray emitters in well as several interesting short period binary sdB+dM NGC 300 (Carpano, Tübingen) and the search for the systems (in collaboration with Solheim, Oslo and Oreiro, missing mass of the Crab Supernova remnant, which has IAC). In collaboration with Telting (NOT) he has presented been an unsolved mystery for more than two decades. the first evidence of line profile variations in an sdB star Deep Hα images have recently been obtained by from time resolved spectroscopy. He has also undertaken Lundqvist et al., and first results look very promising. a survey of spectroscopic subdwarf B binaries with NAOMI in order to put the different evolutionary scenarios Skillen in a collaboration with Pollacco and Todd (QUB), proposed for these stars to a test. Bell (RAL) and Augusteijn (NOT), is conducting an ongoing photometric search for eclipsing binary systems Other projects in this field include mining the Sloan Digital in local group galaxies. Approximately one hundred new Sky Survey for spectroscopic and photometric data on systems have been discovered in each of M31, IC 1613 new and known subdwarf stars, and spectroscopic model and NGC 6822. Selected systems will be followed up fitting of sdB stars and sdB stars in binary systems (with spectroscopically to determine accurately their physical Heber, Bamberg). parameters and hence distances. The goal of this project is to investigate the impact of the physical environment on Østensen has continued to develop a complete database standard candles within the Local Group, and to reduce system for hot subdwarf stars, bringing together results the uncertainty in the determination of the Hubble from the numerous blue star surveys into one searchable Constant to within 5%.
44 • ING BIENNIAL R EPORT 2004–2005 The SuperWASP facility was inaugurated and fully ideas. The outcome prompted new collaborations and commissioned in 2004, in collaboration with Pollacco ideas for observing programmes, while at the same time it (QUB) and the WASP Consortium. The WASP project is provides the observatory with scientifically inspired advice an ultra-wide-angle photometric survey with a precision of on how to maximally exploit the exciting possibilities of AO better than 1% of stars in the magnitude range 7–13, with at the William Herschel Telescope. The proceedings were the primary goal of discovering exosolar planet transits. It published in Rutten, R. G. M., Benn, C. R., Méndez, J., will also provide an unrivalled census of variable stars 2006, New Astronomy Reviews, 49, 487. over the northern sky; the resulting archive will be exploited for a variety of science goals, ranging from the Østensen organized the '2nd Meeting on Hot Subdwarf discovery of exosolar planets to aspects of stellar stars and related objects' at the Real Club Náutico de pulsation, binarity and galactic structure. A programme, in Santa Cruz de La Palma during June 6–10 2005, a collaboration with Barnes (Texas), to determine high precision collaborative venture between the ING and NOT. Hot (0.4 km/s) radial velocity curves of galactic Cepheid stars subdwarf stars are extreme horizontal branch (EHB) stars from echelle spectroscopy, has now been completed. and pre-white dwarf stars. The EHB stars are core helium- burning stars with extremely thin hydrogen envelopes, and form the majority of bright stars in surveys for extremely SCIENTIFIC CONFERENCES blue objects, where they are classified as subdwarf-B (sdB) stars. They also appear in the colour-magnitude Rutten organized the 'Workshop on Adaptive-Optics diagrams of some globular clusters as an extension of the Assisted Integral-Field Spectroscopy' at the Hotel H10 blue tail formed by classical horizontal branch stars, Taburiente Playa in Los Cancajos on La Palma during May though it is not clear why some clusters show this feature 9–11 2005. Integral-field spectroscopy and Adaptive and other do not. The pre-white dwarf stars are related to Optics (AO) techniques are an increasingly important tool the sdBs, but have exhausted their capacity to burn helium in astronomy. A number of integral-field spectrographs are in the core. Many of the brightest hot subdwarfs in the field in operation around the world, and AO instruments are are of this class, and they are classified as sdO stars. proliferating and becoming a standard feature of in particular the largest ground-based telescopes. The Hot subdwarf stars and their relatives are believed to be combination of integral-field spectrographs and AO is still important contributors to the hitherto mysterious UV a relatively unexplored area where the potential benefits upturn phenomenon in early-type galaxies; and a for astronomy are huge. For that reason, a number of comprehensive investigation on this issue is being projects are under way or are being proposed that will take performed by the Galaxy Evolution Explorer (GALEX). The advantage of the most recent technological developments formation of EHB stars remains, in general, a matter of in these areas. The most prominent scientific prospects debate. Recent results for Galactic EHB stars show that are expected to be in the areas of study of the dynamics the majority are close binary stars, so mass transfer and of the central regions of elliptical galaxies and active mass loss due to interactions between the stars clearly galactic nuclei, spectroscopy of gravitationally lensed play a role. EHB stars are an excellent tool for studying high-redshift galaxies, star formation regions and outflow evolution in close binary stars. Some EHB stars shows p- of evolved stars, and the dynamics of crowded stellar fields. mode pulsations with periods of a few minutes and some others show g-mode pulsations with periods on the order The advent of a new facility instrument at the 4.2m William Herschel Telescope, the OASIS Integral Field Spectrograph, working in conjunction with the NAOMI AO system prompted the holding of a workshop covering this area. Moreover, the ING laser guide star facility (GLAS) which is currently under development, will open up nearly the full sky to AO exploitation. This implies a huge new potential for AO assisted spectroscopy to be carried out on large samples of objects, as there no longer will be the restriction of having to have a nearby bright guide star.
The workshop focused on the scientific achievements and prospects of AO-assisted integral field spectroscopy, Figure 57. Group photograph of participants to the workshop on promoting discussion and sharing of experiences and ‘Adaptive-Optics Integral-Field Spectroscopy’.
ING BIENNIAL R EPORT 2004–2005 • 45 of hours. Asteroseismology can be used to measure fundamental parameters for these stars directly. Hot subdwarf stars are also a laboratory for studying the effects of diffusion, weak stellar winds, radiative levitation and gravitational settling. These processes are seen to affect the peculiar composition of their atmospheres and also play a role in the driving mechanism for pulsations and, perhaps, the subsequent evolution of the star.
The meeting was divided into sessions that covered a broad range of topics related to the hot subdwarf stars. They were: evolutionary models and the UV-upturn phenomenon; hot subdwarfs and hot HB stars in the field, clusters and galaxies; atmospheric properties of hot subdwarf stars; hot subdwarfs in binary systems; asteroseismology of sdB stars.
Eight half day sessions were completed during the meeting, with three sessions dedicated to asteroseismology, two sessions for atmospheric properties and the remaining topics filling one session each. 58 participants from all over the world attended the meeting, almost half again as many as at the first meeting. The proceedings are to be published in journal Baltic Astronomy, Volume 15. Figure 58. Announcing poster of the 2nd meeting on ‘Hot Subdawrf Stars and Related Objects’. Danny Lennon organized a Royal Astronomical Society Specialist Meeting 'Science from La Palma —Looking beyond 2009. As part of the decision making process, and Beyond 2009' in collaboration with Evans (ING) and Drew in support of the UK's overall strategic re-evaluation in (ICL). The meeting was held at Burlington House, astronomy, the ING was reviewed during 2005. It was Piccadilly, London, on 14 October 2005. In 2009 the therefore thought timely to assess recent scientific international agreement setting up the Roque de los achievements from the Roque de los Muchachos, and to Muchachos Observatory on the island of La Palma will consider what role the observatory might have beyond have been in existence for a period of 30 years. In the 2009. The meeting was attended by approximately 100 near future the United Kingdom will have to make a astronomers from around the UK, and was structured to decision on whether or not to withdraw from that allow two morning sessions of science talks with agreement and PPARC, through its ownership of the Isaac contributors from various fields in astronomy. This was Newton Group of Telescopes, has the responsibility of followed in the afternoon by a series of strategy talks, deciding on the UK's involvement in the observatory culminating in a half-hour discussion on the future of the ING.
Figure 59. The meeting 'Science from La Palma —Looking Beyond 2009' was held at the lecture theatre of the Geological Society at Burlington House, Piccadilly, London.
46 • ING BIENNIAL R EPORT 2004–2005 Chapter 5
PUBLIC RELATIONS
As in previous years thousands of visitors were shown the WHT and the INT, many as part of the annual observatory open days during the summer, but also through a large number of official visits, of which as much as 40% were schools. In total, ING welcomed 8206 visitors (5656 in 2004 and 2550 in 2005) in 317 tours. Some of our visitors in the reporting period were the Spanish and Dutch ministers of Science and Education and the Spanish astronaut Pedro Duque.
Coinciding with the fiesta of La Bajada de la Virgen de Las Nieves, a new model for organising tours on Open Days in order to reduce the impact on the observatory operations was tested in 2005. Visitors were asked to book online their tours well in advance. The total number of visits per open day was reduced from previous years while increasing the number of days to five.
All these activities help strengthen the ties between the observatory and the public on La Palma. Moreover, apprenticeships for a small number of technical students from La Palma have been hosted by the ING, providing further added value of the observatory to the local community. And ING also helped the foundation of the "Sociedad de Estudios Generales de la Isla de La Palma", Figure 60. Top: Students at the INT control room during WINT a local society devoted to general research of La Palma. observations. Bottom: Students from Marlborough School paying attention to the explanations given by the INT observer. ING continued to provide young highschool students with first contacts with professional telescopes and hands-on and was set up to promote the organization of common experiences, through the participation in night observing. public activities at the Canarian Observatories. Apart from One of the initiatives we supported was "WINT", a Dutch the support to the organization of visits to the ORM and national competition for young students organised by the the Open Days in summer, the group has also printed a NOVA school. Students had to prepare their own collection of brochures for each astronomical facility in observing programmes and the winners were awarded Spanish and in English and it has organized a traveling with two nights on the INT. Another example was from the exhibit that has been displayed at the airport terminals. Marlborough school from the UK, which organised a trip for 5 students and teachers to join the observer at the INT Finally, ING also gave support to the inauguration of for two nights. SuperWASP and for making public the results from Deep Impact at the ING telescopes. Other public activities included the participation of several ING astronomers in the La Palma summer university and ING has been particularly active on scientific outreach in the celebration of the European Science and activities during the reporting period. A workshop on Technology Week in 2004 and 2005. The public outreach "Adaptive-Optics Assisted Integral-Field Spectroscopy" group of OPTICON has members from the CCI institutions was organised on La Palma (9–11 May 2005) which
ING BIENNIAL R EPORT 2004–2005 • 47 Thanks to the collaboration of the observers, we have been able to make available beautiful images, some of which have been awarded the 'NASAAstronomy Picture of the Day' recognition.
A total of 31 press releases have reflected the most relevant research highlights of our scientific production. These press releases were prepared by ING or other institutions and they were based on results from data obtained at the ING telescopes or achieved by ING astronomers. Other contacts with the press included TV teams from Spain, Germany or Ireland that filmed scenes for scientific series or documentaries at the telescopes.
Figure 61. Announcing poster of the workshop on ‘Adaptive-Optics Assisted Integral-Field Spectroscopy’. attracted some 60 participants from around the world. This workshop was inspired by the availability of the OASIS integral field spectrograph on the WHT and of the plans to develop a laser guide star system as well. The proceedings were published in: René, R. G. M., Benn, C., Méndez, J., 2006, New Astronomy Reviews, 49, 487. A joint Isaac Newton Group and Nordic Optical Telescope Conference on "Hot Subdwarf Stars and Related Objects" took place also on La Palma (6-10 June 2005), again with over 60 participants. The proceedings were published in: Østensen, R., 2005, Baltic Astronomy, 15. Both conferences included a public talk and a press conference. And finally a dedicated session focussing on the scientific achievements and the future of the ING was held in London under the auspices of the Royal Astronomical Society.
Four issues of the ING Newsletter and the Biennial Report 2002–2003 were launched in the reporting period. Also remarkable is the large number of requests for using the images and photographs from our public archives in magazines, books, web sites or exhibitions in museums. Figure 62. Top: Image of M81 galaxy obtained using the Wide Field Camera on the INT. Bottom: NGC 7271 galaxy as observed The production of new public astronomical images is of with the Prime Focus camera on the WHT. Both images were vital importance to continue satisfying this high demand. incorporated to ING’s public archive of images.
48 • ING BIENNIAL R EPORT 2004–2005 Appendix A
THE ISAAC NEWTON GROUP OF TELESCOPES
The Isaac Newton Group of Telescopes (ING) consists of the William Herschel Telescope (WHT), the Isaac Newton Telescope (INT) and the Jacobus Kapteyn Telescope (JKT). The WHT, with its 4.2m diameter primary mirror, is the largest in Western Europe. It was first operational in August 1987. It is a general purpose telescope equipped with instruments for a wide range of astronomical observations. The INT was originally used at Herstmonceux in the United Kingdom, but was moved to La Palma in 1979 and rebuilt with a new mirror and new instrumentation. It has a 2.54m diameter primary mirror and is mostly used for wide-field imaging and spectroscopy. The JKT has a primary mirror of 1.0m diameter and it was mainly used for observing relatively bright objects. It ceased science observations in August 2003 and now it is regularly being used for measuring the atmospheric turbulence profile above the observatory. Both the INT and the JKT were first operational in May 1984.
The WHT has an altazimuth mount with a f/2.5 parabolic primary mirror. The WHT is of classical Cassegrain optical configuration. The paraboloidal primary mirror is made of a glass-ceramic material (Cervit) having near-zero coefficient of expansion over the operating temperature range. Instruments can be mounted at the corrected f/2.81 prime focus, f/11 Cassegrain focus, or either of two f/11 Nasmyth foci. The primary mirror is made of a glass-ceramic material (Cervit) having near-zero coefficient of expansion over the operating temperature range, and it weighs 16.5 tonnes. When not operating at prime focus, a convex hyperboloidal secondary mirror, made of Zerodur, 1.0m in diameter, directs the light through a central hole in the primary mirror to the main instrumentation mounted at the Cassegrain focus beneath the primary mirror cell. The telescope also incorporates a third main mirror, a flat, angled at 45 degrees, which can be motor-driven into position at the intersection of the axes, just above the primary mirror, so that the light from the secondary is diverted sideways either through one of the altitude bearings to the Nasmyth platforms.
The INT has a primary mirror with a focal ratio of f/2.94. It uses a polar-disc/fork type of equatorial mount. Instruments can be mounted at the corrected f/3.29 prime or f/15 Cassegrain foci. The optical system of the INT is a conventional Cassegrain with a paraboloidal primary mirror and a hyperboloidal secondary. It weighs 4.4 tonnes and it is made of Zerodur.
The JKT has a parabolic primary mirror of diameter 1.0m and a focal length of 4.596m. It weighs 215kg. It is equatorially mounted, on a cross-axis mount. The JKT has two optical configurations: Harmer-Wynne and Cassegrain. The former one uses a f/8 spherical secondary and the latter one a f/15 hyperbolic secondary. The two optical systems share the same parabolic primary mirror. At present only the Cassegrain configuration is available and instruments mount at the Cassegrain focus.
The following table shows each telescope’s location:
Latitude Longitude Ground floor height WHT 28° 45' 38.3" N 17° 52' 53.9" W 2332m INT 28° 45' 43.4" N 17° 52' 39.5" W 2336m JKT 28° 45' 40.1" N 17° 52' 41.2" W 2364m
The ING operates the three telescopes on behalf of the Particle Physics and Astronomy Research Council (PPARC) of the United Kingdom, the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) of the Netherlands, and the Instituto de Astrofísica de Canarias (IAC) of Spain.
The ING is located at the Observatorio del Roque de Los Muchachos (ORM), on the island of La Palma, Canary Islands, Spain. The ORM, which is the principal European northern hemisphere observatory, is owned by the Instituto de Astrofísica de Canarias. The operation of the site is overseen by an International Scientific Committee, or Comité Científico Internacional (CCI). Financial and operational matters of common interest are dealt with by appropriate subcommittees.
ING BIENNIAL R EPORT 2004–2005 • 49 The observatory also includes the 3.6m Telescopio Nazionale Galileo, the 2.5m Nordic Optical Telescope, the 2.0m Liverpool Telescope, the 1.2m Mercator Telescope, the 60cm telescope of the Swedish Royal Academy of Sciences, the wide-field imaging facility SuperWasp, the Automatic Transit Circle, the 0.97cm New Swedish Solar Telescope, the 45cm Dutch Open Solar Telescope, and the atmospheric imaging Cherenkov 17m Magic Telescopes. Under construction are a twin to the 17m Cherenkov telescope, MAGIC-2, and the 10.4m Gran Telescopio Canarias.
The observatory occupies an area of 1.89 square kilometres approximately 2350m above sea level on the highest peak of the Caldera de Taburiente National Park, in the Palmeran district of Garafía. La Palma is one of the westerly islands of the Canarian archipiélago.
The site was chosen after an extensive search for a location with clear, dark skies all the year around. All tests proved that the Roque de Los Muchachos is one of the best astronomical sites in the world. The remoteness of the island and its lack of urban development ensure that the night sky at the observatory is free from artificial light pollution. The continued quality of the night sky is protected by law. The mountain-top site has a remarkably stable atmosphere, owing to the local topography. The mountain has a smooth convex contour facing the prevailing northerly wind and the air-flow is comparatively undisturbed, allowing sharp and stable images of the night sky.
Many of the state-of-art telescope and instrument components are custom-built. New instruments are designed and built by technology groups mainly in the United Kingdom, the Netherlands, and Spain, with whom the ING maintains close links, and by astronomers and engineers working at ING.
THE INTERNATIONAL AGREEMENTS
The international agreements by which the Roque de Los Muchachos and the Teide Observatories were brought into existence were signed on La Palma on 26 May 1979. The participant nations at that time were Spain, the United Kingdom, Sweden and Denmark. Later other European countries also signed the agreements. Infrastructural services including roads, communications, power supplies as well as meals and accommodation facilities have been provided by the Spanish side. In return for the use of the observatory and its facilities all foreign user institutions make 20 per cent of time on their telescopes available to Spanish observers. Representatives of the participant institutions meet together as the International Scientific Committee, or Comité Científico Internacional (CCI).
The inauguration of the Canary Islands observatories took place on 29 June 1985 in the presence of the monarchs and members of the Royal Families of five European countries, and the Presidents of another two.
THE ING BOARD AND THE DIRECTOR’S ADVISORY COMMITTEE
The PPARC, the NWO and the IAC have entered into collaborative agreements for the operation of and the sharing of observing time on the ING telescopes. The ING Board was set up to oversee the operation of this agreement, to foster and develop collaboration between astronomers of the United Kingdom, the Netherlands and Spain, and to ensure that the telescope installations are maintained in the forefront of world astronomy. In particular, the ING Board oversees the programme of instrumentation development, determines the programme of operation and maintenance of the installations, approves annual budgets and forward estimates and determines the arrangements for the allocation of observing time.
The Director’s Advisory Committee (DAC) assists the observatory in defining the strategic direction for operation and development of the telescopes. It also provides an international perspective and acts as an independent contact point for the community to present its ideas. The ING Board at the Gran Telescopio Canarias.
50 • ING BIENNIAL R EPORT 2004–2005 TELESCOPE TIME AND DATA OWNERSHIP
The construction, operation, and development of the ING telescopes is the result of a collaboration between the United Kingdom, the Netherlands and Spain. The site is provided by Spain, and in return Spanish astronomers receive 20 per cent of the observing time on the telescopes. A further 75 per cent is shared by the United Kingdom, the Netherlands and the IAC. The remaining 5 per cent is reserved for large scientific projects to promote international collaboration between institutions of the CCI member countries. It is intended that this time be used for the study of one, or a few, broad topics each year by several telescopes. This time is allocated by the CCI.
It is the responsibility of the IAC to make the Spanish time available to Spanish institutions and others, via the Comité para la Asignación de Tiempos (CAT). The ING Board has delegated the task of time allocation to British and Dutch astronomers to the PPARC Panel for the Allocation of Telescope Time (PATT) and the NFRA Programme Committee (PC) respectively. All the above agreements envisage that observing time shall be distributed equitably over the different seasons of the year and phases of the Moon.
Notwithstanding the above, any astronomer, irrespective of nationality or affiliation, may apply for observing time on the ING. Astronomers who are working at an institute in one of the partner countries should apply through the route appropriate to their nationality or the nationality of their institute.
Time is allocated in two semesters, from 1 February to 31 July (semester A) and from 1 August to 31 January (semester B). Decisions on time allocations are made on the basis of scientific merit and technical feasibility of the proposed observations.
ING policy is that data belongs exclusively to those who collected it for a period of one year, after which it is available in a common archive for all astronomers (http://archive.ast.cam.ac.uk/ingarch/). It may be used at any time for engineering or instrumental investigations in approved programmes carried out to improve facilities provided at the observatory.
Service observations which are made by support astronomers at the request of others are similarly treated. However, calibration data may well be used for more than one observation and may therefore be available in common to several groups. It may happen that identical or similar service observations are requested by two or more groups. Requests which are approved before the data are taken may be satisfied by requiring the data to be held in common by the several groups. It is up to them how they organise themselves to process, analyse, relate to other work, and eventually publish the data.
Requests for observations from programmes already executed on the telescopes should be referred to the original owners of the data, and/or to the data archive. This is the policy whether or not the data were obtained by PATT, NFRA PC, or CAT scheduled astronomers, or by service requests.
ING BIENNIAL R EPORT 2004–2005 • 51 Appendix B
TELESCOPE INSTRUMENTATION
The design of the WHT allows great flexibility in instrumentation as this telescope allows fast and easy switching between the Cassegrain and Nasmyth foci. For this reason, and to take advantage of the large light collecting power of this telescope, operation and developmental efforts focus on the WHT. Also visiting instruments, i.e. instruments built and used by external groups for their own use, are welcome at the WHT and have attracted a great deal of attention. The INT is equipped with only one instrument, the Wide Field Camera. A broad functional division in instrumentation capability between the WHT and INT is as follows:
William Herschel Telescope Optical pectroscopy and spectro-polarimetry over a wide range of resolving powers Imaging polarimetry IR spectroscopy Multi-object spectroscopy Areal spectroscopy Optical and infrared imaging High spatial resolution imaging Coronography
Isaac Newton Telescope CCD imaging
The following table summarises the common-user instruments which were available during 2004 and 2005:
Focus Instrument Detector
William Herschel Telescope
Cassegrain ISIS double spectrograph EEV and Marconi CCDs Auxiliary port camera (AUX) Tektronix CCD IR imager and spectrograph (LIRIS) Rockwell HgCdTe array
Nasmyth Adaptive optics instrumentation: NAOMI / INGRID / OSCA Rockwell HgCdTe array NAOMI / OASIS MIT/LL CCD
Prime Prime Focus imaging Camera (PFIP) 2 × EEV CCD Autofib Fibre Positioner (AF2) and WYFFOS spectrograph 2 × EEV CCD
Isaac Newton Telescope
Prime Wide Field Camera (WFC) 4 × EEV CCDs
52 • ING BIENNIAL R EPORT 2004–2005 Appendix C
STAFF ORGANISATION
DIRECTORATE D. Mislis (from 06.10.03 to 13.09.2004) R. Parker (from 26.08.2005) R. G. M. Rutten, Director D. Russell (from 11.08.03 to 11.08.2004) L. Sabin (from 19.08.2005) ADMINISTRATION S. Simon (from 01.10.2004 to 30.09.2005) E. C. Barreto N. Styles (from 15.09.03 to 31.05.2004) L. I. Edwins, Head of Administration N. L. González ENGINEERING L. A. Lawler (until 23.10.2005) R. G. Talbot, Head of Engineering J. Martínez B. van der Elst (to 31/03/2004) Computing P. v. d. Velde D. C. Abrams, Group Leader Students: D. Armstrong (to 30.04.2004) E. C. Barnett (until 20.08.2004) R. Bassom (to 30.06.2005) V. H. Jones (from 09.09.2005) C. Bevil J. Keable (from 20.09.2004 to 19.08.2005) S. Goodsell (to 31.07.2004) F. J. Gribbin ASTRONOMY L. Hernández G. F. Mitchell C. R. Benn A. d. Paz (from 20.09.2004 to 19.12.2004) R. Corradi S. Picó (from 01.09.2004) R. Greimel J. Piñero P. Leisy S. G. Rees D. J. Lennon, Head of Astronomy J. Skvarc (from 05.01.2005) J. Licandro J. Méndez Note: During the period covered by this report the R. Østensen Computing Facilities and the Software Groups joined to a S. Rix (from 01.06.2004) new group, the Computing Group. M. Schirmer (from 01/03/2004) W. J. I. Skillen Telescopes & Instrumentation A. Zurita (to 31/01/2004) N. Apostolakos (from 01.10.2004) PPARC Postdoc: C. Benneker (to 30.09.2004) C. Evans (from 14.01.2002 to 14/10/2005) M. Blanken D. Cano (from 01.09.2004), Group Leader Students: T. S. Gregory P. Behrens (from 26.08.2005) A. K. Hide (to 30.04.2004), Group Leader A. Cardwell (from 29.08.2005) M. v. d. Hoeven J. Furness (from 01.09.2004 to 30.08.2005) C. W. M. Jackman (to 15.03.2004) A. García (from 01.09.02 to 31.08.2004) P. D. Jolley S. Hickey (from 05.09.2005) O. Martin (from 09.05.2003) M. Jaigirdar (from 01.09.2004 to 29.08.2005) A. Ridings F. Monterrey (05.2003) S. M. Tulloch
ING BIENNIAL R EPORT 2004–2005 • 53 Student: Student: N. Apostolakos (to 30.09.2004) J. Hutchinson (from 14.05.2004 to 14.09.2004)
OPERATIONS TEAM Telescope Operators
A. K. Chopping J. N. González J. R. Concepción J. C. Guerra (from 01.08.2004) K. M. Dee, Head of Operations C. Martín J. M. Díaz N. O’Mahoney D. González A. Guillén D. Gray (to 26.09.2004) R. Martínez J. C. Pérez R. Pit J. Rey (from 01.08.2004), Group Leader S. Rodríguez
54 • ING BIENNIAL R EPORT 2004–2005 Appendix D
TELESCOPE TIME AWARDS
The UK Panel for the Allocation of Telescope Time (PATT), the Dutch NFRA Programme Committee (PC), the Spanish Comité para la Asignación de Tiempos (CAT) and the Comité Científico Internacional (CCI) made time awards to the following observing proposals in 2004 and 2005. The principal applicant, his or her institution or university, the title of the proposal, and the proposal reference are listed below. Semester A runs from February to July and semester B from August to January.
SEMESTER 2004A
William Herschel Telescope
UK PATT
– Charles (Southampton). Determining system parameters of a soft X-ray transient in outburst. W/2004A/36 – Charles (Southampton). The mass donor in SS43. W/2004A/56 – Harries (Exeter). Spectropolarimetry of symbiotic binaries. W/2004A/6 – Haswell (OU). Accretion disc precession in AM CVn. W/2004A/49 – Hodgkin (IoA). Spectroscopic identification of very low-mass stars and brown dwarfs in young open clusters. W/2004A/54 – Jarvis (Oxford). Quantifying the space density of radio-loud quasars at z>5. W/2004A/19 – Jeffery (Armagh). PG1544+488 and other helium-rich subdwarfs: binaries, mergers or bizarre. W/2004A/45 – Keenan (QUB). The space density of B-type stars in the Galactic halo. W/2004A/3 – Lucas (Hertfordshire). PLANETPOL polarimetry of Tau Boo Ab. W/2004A/27 – Marsh (Warwick). ULTRACAM observations of detached white dwarf/M dwarf binary stars. W/2004A/35 – Meikle (ICL). Direct detection and study of supernovae in nuclear starbursts. W/2002B/56 LT – Meikle (ICL). Detailed study of the physics of nearby Type Ia supernovae. W/2003B/2 LT – Merrifield (Nottingham). Determining the dynamics of round elliptical galaxies using the Planetary Nebula Spectrograph. W/2003A/38 LT – Miller (Oxford). A deep survey for cluster-lensed QSOs from SDSS and 2QZ. W/2004A/58 – O’Brien (Leicester). Optical identification of ultra-soft X-ray sources —searching for extreme accretion. W/2004A/32 – Østensen (ING). Resolving sdB binary systems with Adaptive Optics. W/2004A/46 – Rawlings (Oxford). FLAGS — understanding the starburst-AGN connection. W/2004A/17 – Roques (Observatoire de Paris). Search for small Kuiper Belt objects by stellar occultations. W/2004A/38 – Smail (Durham). A Lyman-break survey in the SCUBA/BLAST region. W/2004A/8 – Smith (Sussex). Mapping the surface of the secondary stars in cataclysmic binaries. W/2004A/50 – Snellen (IoA). The space-density of high redshift FRI radio galaxies (II). W/2004A/23 – Vink (ICL). Searching the environments of Herbig Be stars for clusters and discs. W/2004A/39 – Wilkinson (IoA). Dark matter in the Sextans dwarf spheroidal. W/2004A/2
NL NFRA PC
– Cole (Groningen). Calcium triplet spectroscopy of Galactic open clusters. w04an005 – Douglas (Groningen). Determining the dynamics of round elliptical galaxies using the Planetary Nebula Spectrograph (PN.S). w04an012 – Groot (Nijmegen). The missing link of cataclysmic variable evolution in the Sloan Digital Sky Survey? w04an013 – Groot (Nijmegen). High speed spectral eclipse mapping of accretion disks in cataclysmic variables. w04an014 – Groot (Nijmegen). High speed spectral eclipse mapping of accretion disks in cataclysmic variables. w04an017 – Nagar (Groningen). Sub-kiloparsec kinematics in Seyferts and non-active galaxies — a comparative study. w04an006 – Perryman (ESTEC). Testing the relation between magnetic field strength and QPO frequency in polars. w04an003 – Perryman (ESTEC). The optical counterparts of radio pulsars. w04an004 – Quirrenbach (Leiden). Line bisector variations for K giant stars with possible planetary companions. w04an015 – Roelofs (Nijmegen). Measuring directly the anticipated tidal deformation of the accretion disk of AM CVn. w04an010 – Röttgering (Leiden). Multi-object spectroscopy of radio sources in the Bootes Deep Field. w04an008 – van der Klis (Amsterdam). Comparing a neutron star with two black hole transients in quiescence. w04an002 – Wijers (Amsterdam). The nature of Gamma-Ray Bursts and their use as cosmological probes. w04an011
ING BIENNIAL R EPORT 2004–2005 • 55 SP CAT
– Alonso (IAC). Adaptive Optics observations of candidates to transiting extrasolar planets. W29/2004 – Beckman (IAC). Vertical structure of nuclear bars in double-bar galaxies. W11/2004A – Beckman (IAC). Evolution of galactic star formation: the morphologic method. W37/2004A – Casares (IAC). Echo tomography of fluorescence lines in Sco X-1. W35/2004A – Casares (IAC). Determining system parameters of a Soft X-ray transient in outburst. W36/2004A – Castander (IEEC). Spectroscopy of pairs of quasars in the line-of-sight: a study of the proximity effect. W39/2004A – Castro-Tirado (IAA). The nature of Gamma-Ray Bursts (GRBs). W33/2004A – Díaz (UAM). Spectrophotometry of the brightest HII galaxies from the SDSS. W23/2004A – Erwin (IAC). How many galactic bulges are imposters? W5/2004A – González (IAC). Searching for the evidence of a supernova event in the LMXB V404Cyg. W21/2004A – Gutiérrez (IAC). Systems with anomalous redshifts. W19/2004A – Martín (IAC). Spectroscopic identification of very low-mass stars and brown dwarfs in young open clusters. W3/2004A – Martínez (Valencia). Properties of the haloes around field elliptical galaxies. W30/2004A – Pascual (UCM). Physical properties and chemical abundances of the population of current star-forming galaxies at z=0.24. W16/2004A – Pérez (IAA). Massive stellar clusters in nearby disc galaxies. W40/2004A – Pohlen (IAC). A test of the bar-peanut connection in a bulge-less galaxy. W7/2004A – Rebolo (IAC). Direct detection of giant exoplanets and brown dwarfs around young nearby stars. W17/2004A – Ruiz (Barcelona). Supernovae at z=0.35–0.65: a study of the nature of the dark energy. W1/2004A – Santander (IAC). The origin of extended nebulae around symbiotic stars. W20/2004A – Vazdekis (IAC). Ages and metallicities of S0 galaxies along the Colour-Magnitude relation. W25/2004A
Spanish Additional Time
– Balcells (IAC). U-band deep survey for COSMOS and OTELO. W9/2004A – Cepa (IAC). The OTELO project: deep BVRI survey of Groth and SIRTF-FLS fields. W27/2004A
TNG-TAC
– Fasano (Padova). Star formation and morphological evolution of galaxies in nearby clusters with WYFFOS. T064
Isaac Newton Telescope
UK PATT
– Alton (CEA Saclay). The dust-to-gas ratio of the intergalactic gas in the M81 group. I/2004A/1 – Cotter (Oxford). A complete investigation of low-redshift radio galaxies and their cluster environments. I/2004A/20 – Davies (Cardiff). Satellites in nearby galaxy halos (M101). I/2004A/3 – de Blok (Cardiff). Deep BVRI surface photometry of core-dominated low surface brightness galaxies. I/2004A/12 – Drew (ICL). IPHAS — the INT/WFC photometric Hα survey of the northern galactic plane. I/2004A/8 – Feltzing (Lund). A differential study of the metallicity distribution functions in three northern dwarf spheroidal galaxies. I/2004A/9 – Fitzsimmons (QUB). Rapid-response astrometry of potentially hazardous asteroids. I/2004A/6 – Helmi (Groningen). Star streams and High Velocity Clouds in the Milky Way halo. I/2004A/23 – Hewett (IoA). Faint planetary nebulae around hot white dwarfs. I/2004A/11 – Jarvis (Oxford). A wide-field search for Ly-α haloes: A pre-requisite for massive galaxy formation. I/2004A/17 – Jarvis (Oxford). Quantifying the space density of radio-loud quasars at z>5. W/2004A/19 [sic] – Snellen (IoA). The space-density of high redshift FRI radio galaxies. I/2004A/5
NL NFRA PC
– Aragon (Groningen). Measuring galaxy spin alignments along a void-intersection filament near AWM3. i04an007 – Braun (NFRA). The STARFORM/Hα survey: Probing the recent history of star formation in spirals. i04an003 – Habing (Leiden). Monitoring of Asymptotic Giant Branch stars in Local Group Galaxies. i04an001 – Oosterloo (NFRA). The mass distribution in extremely warped disk galaxies. i04an006 – Röttgering (Leiden). A survey for Ly-α emission line halos and the properties of z>2 proto-clusters. i04an008 – Wijers (Amsterdam). The nature of Gamma-Ray Bursts and their use as cosmological probes. w04an011 [sic]
UK/NL WFS Programmes
– Casares (IAC). The orbital parameters of XTE J1859+226. I10/2004A – Castro-Tirado (IAA). The nature of Gamma-Ray Bursts (GRBs). W33/2004A [sic] – Deeg (IAC). Sample definition for exoplanet detection by the COROT space craft. I13/2004A
56 • ING BIENNIAL R EPORT 2004–2005 – Erwin (IAC). The outer disks of S0 galaxies: clues to disk evolution. I3/2004A – Gómez-Flechoso (UEM). Constraining the shape of the Milky Way dark matter halo with the Sgr tidal stream. I12/2004A – Gutiérrez (IAC). Searching for Sunyaev-Zeldovich Clusters. I8/2004A – Hammersley (IAC). A deep multi-wavelength survey of the Galactic Plane. I9/2004A – Leisy (IAC/ING). IPHAS — the INT/WFC photometric Hα survey of the Northern Galactic Plane. I4/2004A – López (IAC). Quantitative morphology of Hercules galactic supercluster. I1/2004A – López (IAC). Tracing the intracluster light in Virgo Cluster. I2/2004A – Mampaso (IAC). Planetary nebulae and the intergalactic stellar population in the intragroup medium. I6/2004A – Vázquez (IAC). Stellar and solar oscillations. I5/2004A
Spanish Additional Time
– Herrero (IAC). Detecting the population of blue massive stars to 5 Mpc for OSIRIS. I11/2004A – Vílchez (IAA). An Hα search for star-forming galaxies in nearby clusters. I14/2004A
SEMESTER 2004B
ITP Programmes on the ING Telescopes
– Gäensicke (Warwick). Towards a global understanding of close binary evolution. ITP7
William Herschel Telescope
UK PATT
– Bunker (Exeter). Star formation at redshift ~1. W/2004B/56 – de Blok (Cardiff). Deep K-band surface photometry of low surface brightness galaxies. W/2004B/30 – Dhillon (Sheffield). ULTRACAM observations of the transiting extrasolar planet HD209458b. W/2004B/14 – Dufton (QUB). Spectroscopy of h+c Persei to support VLT/FLAMES survey of the Magellanic Clouds (payback). W/2003B/3 – Gaensicke (Warwick). HS2331+3905: A cataclysmic variable in its final days? W/2004B/37 – Hirtzig (Meudon). Titan’s surface and atmosphere: in-depth diagnostic via spectro-imagery. W/2004B/69 – Jeffers (St Andrews). High-resolution Doppler imaging of RS CVn SV Cam. W/2004B/33 – Jeffery (Armagh). Mode identification from multicolour photometry of the pulsating sdB star PG 0014+067. W/2004B/44 – Knigge (Southampton). Spectroscopic reconnaissance of candidate emission line stars discovered by IPHAS. W/2004B/71 – Kotak (ICL). Optical spectroscopic study of the physics of nearby Type Ia Supernovae. W/2004B/16 – Kotak (ICL). Optical spectroscopic study of the physics of nearby Type Ia Supernovae. W/2004B/17 – Leven (Leicester). GRBs as cosmological probes. W/2004B/60 – Littlefair (Exeter). The quiescent accretion disc in the dwarf nova IP Peg. W/2004B/31 – Lucas (Hertfordshire). PLANETPOL polarimetry of Upsilon Andromedae b. W/2004B/6 – Marsh (Warwick). Stochastic Variability of Accreting White Dwarfs. W/2004B/21 – Marsh (Warwick). Magnetism in “non-magnetic” cataclysmic variable stars. W/2004B/66 – Maxted (Keele). Eclipsing binaries in open clusters — spectroscopy. W/2004B/40 – McLure (IoA). Exploring the connection between bulge/black-hole mass and radio luminosity from z=0 to z=2. W/2004B/34 – Meikle (ICL). Late-time study of the nearby type IIP Supernova 2004am. W/2004B/38 – Meikle (ICL). Direct detection and study of supernovae in nuclear starbursts. W/2002B/56 LT – Merrifield (Nottingham). Gravitational redshift in M32 and the properties of its stellar population. W/2004B/39 – Nelemans (IoA). Testing common envelope theory and SN Ia progenitor models with double white dwarfs. W/2004B/47 – Royer (Leuven). A complete survey of the Wolf-Rayet content of M33. W/2004B/28 – Smith (Hertfordshire). The high and low ionization broad-line region in quasars. W/2004B/5 – Tanvir (Hertfordshire). The physics of short bursts and relativistic blast waves. W/2004B/51 – Vink (ICL). A search for evidence of accretion in Herbig Be stars. W/2004B/4 – Wilkinson (IoA). Dark matter in the Sextans dwarf spheroidal. W/2004B/70
NL NFRA PC
– Aerts (Nijmegen). Asteroseismology of the pulsating sdB star PG 0014+067. w04bn015 – de Zeeuw (Leiden). Mapping the nuclear regions of SAURON early-type galaxies with OASIS. w04bn006 – Franx (Leiden). Infrared Spectroscopy of restframe Optically Red Galaxies at high redshift. w04bn008 – Groot (Nijmegen). Spectroscopic reconaissance of emission line stars discovered by IPHAS. w04bn013 – Groot (Nijmegen). The UV-excess and White Dwarf binary population in the Faint Sky Variability Survey. w04bn014 – Groot (Nijmegen). The missing link of Cataclysmic Variable evolution in the Sloan Digital Sky Survey? w04bn016 – McDermid (Leiden). Black hole masses from gaseous and stellar kinematics using OASIS+NAOMI. w04bn007
ING BIENNIAL R EPORT 2004–2005 • 57 – Nelemans (Nijmegen). Testing common envelope theory and SN Ia progenitor models with double white dwarfs. w04bn004 – Nelemans (Nijmegen). The masses of millisecond pulsars. I. Identification of suitable white dwarf companions. w04bn005 – Quirrenbach (Leiden). Line bisector variations for K giant stars with possible planetary companions. w04bn011 – Trager (Groningen). The stellar populations of gas-selected early-type galaxies. w04bn003 – Wijers (Amsterdam). GRBs as cosmological probes. w04bn009 – Wijers (Amsterdam). The physics of short bursts and relativistic blast waves. w04bn012
SP CAT
– Arribas (STScI/IAC). The potential of Integral Field Spectroscopy detecting extrasolar planetary features: INTEGRAL observations of HD209458b. W28/2004B – Cairós (IAC). Multiwavelength studies of metal-poor Blue Compact Dwarf Galaxies: unveiling their evolutionary state. W33/2004B – Casares (IAC). Determining system parameters of a soft X-ray transient in outburst. W2/2004B – Castro-Tirado (IAA-CSIC). The nature of Gamma-Ray Bursts (GRBs). W36/2004B – Colina (IEM/CSIC). INTEGRAL study of very luminous infrared galaxies. W4/2004B – Exter (IAC). Searching for chemical inhomogeneities in planetary nebulae (PNe). W18/2004B – Gallego (UCM). The evolution of the star formation rate density of the Universe up to z=0.8. W45/2004B – González (IAC). Probing the evidence of a supernova event in the black hole binary A0620-00. W12/2004B – Hatzidimitriou (Creta). Identification of optical counterpart X-ray sources in M33. W5/2004B – Iglesias (Marseille). Galactic stellar formation in nearby clusters. W21/2004B – Magrini (Firenze). The chemical composition of HII regions in M33. W16/2004B – Martínez (Valencia). The mass and the extension of the haloes of elliptical galaxies. W10/2004B – Martínez-Delgado (IAC). Does M31 have as many satellites as predicted by Cold Dark Matter theory? W37/2004B – Miranda (IAC). Fluorescence processes in astrophysics: the excitation of OI 8446. W20/2004B – Santander (IAC). The dynamic structure and evolution of Nova Persei 1901 remnant. W6/2004B – Shahbaz (IAC). Infrared spectroscopy of black hole X-ray transients: accurate mass determinations. W34/2004B – Vazdekis (IAC). Using late-type spirals as a probe of galaxy formation. W39/2004B – Zurita (Granada). Spectroscopic identification of Hα emitters discovered by IPHAS. W30/2004B
Spanish Additional Time
– Balcells (IAC). The GOYA sample. Photometric characterisation of high-redshift galaxies. W46/2004B – Cepa (IAC/ULL). The OTELO project: Deep B,V,R,I survey of SA68 and VIRMOS-0226 fields. W22/2004B – Corral (IAC/GTC). Luminous blue stars in M33. W51/2004B – Herrero (IAC). Detecting the population of blue massive stars to 5 Mpc for OSIRIS. W50/2004B – Manchado (IAC). LIRIS GT
TNG-TAC
– Boschin (Trieste). Radio-halo clusters and cluster mergers: a homogeneous dynamical analysis of a large Northern sample. T29 – Fasano (OAP). Star formation and morphological evolution of galaxies in nearby clusters with WYFFOS. T12 – Galleti (Bologna). The Globular Cluster system of M31: a radial velocity survey for 86 candidates and the M31 total mass. T37
Instrument Builder’s Guaranteed Time
– Bacon (Lyon). OASIS. GT Type A – Bacon (Lyon). OASIS. GT Type B
Isaac Newton Telescope
UK PATT
– Aigrain (IoA). Searching for planetary transits in the Orion Nebula Cluster. I/2004B/19 – Dowsett (IoA). A systematic study of AGN within distant galaxy clusters. I/2004B/18 – Drew (ICL). IPHAS: the INT/WFC photometric Hα survey of the northern galactic plane. I/2004B/10 – Jarvis (Oxford). A wide-field search for Lyman-α haloes: A pre-requisite for massive galaxy formation? I/2004A/17 LT – Littlefair (Exeter). How long do young stars remain locked to their discs? I/2004B/14 – McMahon (IoA). Photometric calibration of the XMM-Newton Serendipitous Survey Imaging Program. I/2004B/23 – Murphy (IoA). Testing CDM with galaxy rotation curves at large impact parameters. I/2004B/4 – Rawlings (Oxford). Tracing star-formation in two forming superstructures. I/2004B/7 – Vlahakis (Cardiff). The optically-selected SLUGS: A systematic survey of the Local Submillimetre Universe. I/2004B/13
58 • ING BIENNIAL R EPORT 2004–2005 NL NFRA PC
– Aragon (Groningen). Measuring galaxy spin alignments along the Pisces-Perseus ridge in the vicinity of A262. i04bn001 – Braun (NFRA). The STARFORM/Hα survey: Probing the recent history of star formation in spirals. i04bn004 – Groot (Nijmegen). IPHAS: the INT/WFC photometric Hα survey of the northern galactic plane. i04bn006 – Groot (Nijmegen). A HeI survey of the Galactic Plane: The AM CVn population. i04bn007 – Helmi (Groningen). The role of minor mergers in the build up of the Milky Way halo. i04bn003
SP CAT
– Barrena (IAC). Photometric and morphologic characterisation of galactic clusters with diffuse radio and X-ray emission. I7/2004B – Beckman (IAC). The links between bars and star formation: An advanced survey. I10/2004B – Castro-Tirado (IAA-CSIC). The nature of Gamma-Ray Bursts (GRBs). W36/2004B [sic] – Deeg (IAC). Sample definition for exoplanet detection by the COROT space craft. I9/2004B – Leisy (IAC/ING). IPHAS: the INT/WFC photometric Hα survey of the northern galactic plane. I6/2004B – López (IAC). Diffuse light in compact galactic clusters. I5/2004B – Negueruela (Alicante). Optical counterparts to Newton-XMM sources in open clusters. I3/2004B – Rosenberg (IAC). Formation and evolution of the Milky Way (III): The Galactic disc. I8/2004B
Spanish Additional Time
– Barrado (LAEFF-INTA). Exploring the different IMFs in the Lambda Ori SFR. I1/2004B – Herrero (IAC). Detecting the population of blue massive stars to 5 Mpc for OSIRIS: making a complete sample of M33 population. I11/2004B – Vílchez (IAA). A Deep search for star-forming galaxies in nearby clusters. I4/2004B
SEMESTER 2005A
ITP Programmes on the ING Telescopes
– Gänsicke (Warwick). Towards a global understanding of close binary evolution. ITP7.
William Herschel Telescope
UK PATT
– Ahmad (Armagh Observatory). Parameters of hot subdwarfs of the double-lined spectroscopic binary — PG 1544+488. W/2005A/46. – Bailey (AAO). A high precision polarization survey of bright stars. W/2005A/10. – Blundell (Oxford). A complete spatial and dynamical study of the microquasar SS433. W/2005A/52. – Bower (Durham). The Lyman-α haloes of SCUBA galaxies: exploring super-winds and feedback at z=3. W/2005A/21. – Christian (Queen’s University Belfast). ISIS characterisation of variable stars from the SuperWASP survey. W/2005A/36. – Dobbie (Leicester). A rigorous examination of the evolutionary status of SDSS hot DB white dwarfs within the DO/DB gap. W/2005A/5. – Gänsicke (Warwick). SW, Sextantis stars — totally normal? W/2005A/31. – Hewett (IoA, Cambridge). Imaging of spectroscopically selected gravitational lenses from the SDSS. W/2005A/19. – Hough (Hertfordshire). Circular spectropolarimetry of DIBs. W/2005A/7. – Jarvis (Oxford). Spectroscopic redshifts for the first radio galaxy sample selected at 74 MHz. W/2005A/8. – Keenan (Queen’s University Belfast). The space density of B-type stars in the Galactic halo. W/2005A/6. – Knigge (Southampton). Spectroscopic reconnaissance of candidate emission line stars discovered by IPHAS. W/2005A/39. – Kosroshah (Birmingham). A membership study of the nearest fossil group. W/2005A/17. – Kurosawa (Exeter). The clumpy nature of O supergiant stellar winds. W/2005A/42. – Levan (Leicester). Probing the high redshift universe with GRBs. W/2005A/53. – Lucas (Hertfordshire). PLANETPOL polarimetry of Tau Boo Ab. W/2005A/20. – Magrini (Firenze, Italy). The chemical content of nearby galaxies: GR 8. W/2005A/29. – Merrifield (Nottingham). Determining the dynamics of round elliptical galaxies using the Planetary Nebula Spectrograph. W/2005A/37. – Pettini (IoA, Cambridge). The nature of DLA galaxies traced through spin temperatures: the optical survey. W/2005A/3. – Pozzo (ICL). Late-time study of the very nearby Type IIP SN 2004dj. W/2005A/13. – Tadhunter (Sheffield). Ultraluminous infrared galaxies: quasars and radio galaxies in the making? W/2005A/1. – Tanvir (Hertfordshire). The physics of short bursts and relativistic blast waves. W/2004B/51 LT. – Wilkinson (IoA, Cambridge). Dark matter at the edge of the Sextans dwarf spheroidal. W/2005A/35.
NL PATT
– Cappellari (Leiden Observatory). Dark matter in early-type galaxies: stellar line-of-sight velocity-distribution at 5Re using SAURON. w05an005.
ING BIENNIAL R EPORT 2004–2005 • 59 – Douglas (Kapteyn Institute). Determining the dynamics of round elliptical galaxies using the Planetary Nebula Spectrograph (PN.S). w05an014. – Franx (Leiden Observatory). Infrared spectroscopy of restframe optically red galaxies at high redshift. w05an006. – Groot (Nijmegen). High-resolution eclipse mapping of accretion disks in cataclysmic variables. w05an004. – Helmi (Kapteyn Institute). Building up the Milky Way halo via accretion of small satellites. w05an017. – McDermid (Leiden Observatory). The central black hole in NGC 4486A: measuring the mass and environment with OASIS+NAOMI. w05an023. – Roelofs (Nijmegen). Measuring directly the anticipated tidal deformation of the accretion disk of AM CVn. w05an012. – Wijers (Amsterdam). The physics of short bursts and relativistics blast waves. w05an013. – Wijers (Amsterdam). Probing the high redshift universe with GRBs. w05an020.
SP CAT
– Beckman (IAC). Basic properties of the nuclear bars in galaxies with double bar. W39/2005A. – Cairós (IAC). Near infrared mapping of blue compact dwarf galaxies: disentangling the starburst and the old stars. W33/2005A. – Casares (IAC). Determining system parameters of a Soft X-ray transient in outburst. W1/2005A. – Eiroa (Autónoma de Madrid). IMF to the subestellar limit in extremely young pre-main sequence clusters: Serpens. W14/2005A. – González (IAA). Finding an evolutionary link between radio galaxies and very luminous infrared galaxies. W8/2005A. – Gorgas (Complutense de Madrid). The star formation history of elliptical galaxies in different environments. W52/2005A. – Licandro (IAC/ING). The Deep Impact experiment. W19/2005A. – López (IAC). Studying the dynamics and origin of nuclear bars. W38/2005A. – López-Martín (IAC). Identifying and characterising the counterparts to ULXs. W30/2005A. – López-Sánchez (IAC). Star formation zones in starburst galaxies with tidal streams. W51/2005A. – Mediavilla (IAC). Photometric and spectroscopic variability of gravitational lenses. WL2/2005A. – Mollá (CIEMAT, Madrid). Stellar populations in cooling flow cluster galaxies. W22/2005A. – Pérez (Autónoma de Madrid). Propagation of star formation in apparently compact blue galaxies. W29/2005A. – Rodríguez (Vigo). Physical parameters and chemical abundances in hot type O subdwarfs. W26/2005A. – Shahbaz (IAC). The origin of the optical variability in the black hole X-ray transient V404 Cyg. W50/2005A. – Zapatero (LAEFF-INTA). Brown dwarfs around poor metallicity stars. W21/2005A. – Zeilinger (Institute for Astronomy, Viena). Ram-pressure stripping in Virgo cluster galaxies and their extraplanar ionised gas. W56/2005A.
Spanish Additional Time
– Balcells (IAC). GOYA deep infrared survey. W41/2005A. – Hammersley (IAC). Visible spectroscopy of the GTC standards. W31/2005A. – Herrero (IAC). Detecting the population of blue massive stars to 5 Mpc for OSIRIS. W40/2005A. – Martín (IAC). A search for brown dwarf candidates in three young open clusters for GTC follow-up. W3/2005A.
WHT–TNG Time Share
– Jeffers (Observatoire Midi-Pyrenees, France). Starspot tracking on the W Ursae Majoris system 44 Boo. W/2005A/24 [on the TNG]. – Quirrenbach (Leiden Observatory). Line bisector variations for K giant stars with possible planetary companions. w05an001 [on the TNG]. – Trevese (Roma). Investigating the nature of Low Luminosity Active Galactic Nuclei (LLAGN). T15 [on the WHT].
Instrument Builders' Guaranteed Time
– Bacon (CRAL-Observatoire, Lyon). GT Type A. – Bacon (CRAL-Observatoire, Lyon). GT Type B. – Manchado (IAC). LIRIS GT.
Isaac Newton Telescope
UK PATT
– Burleigh (Leicester). Faint planetary nebulae around hot white dwarfs. I/2005A/8. – Coates (MSSL). Wide-field imaging of Comet 9P/Tempel during the Deep Impact collision. I/2005A/11. – Drew (ICL). IPHAS — the INT/WFC photometric Hα survey of the northern galactic plane. I/2005A/7. – James (Liverpool John Moores). Star formation history of dwarf galaxies in the Virgo cluster. I/2005A/6. – Jarvis (Oxford). A wide-field search for Lyman-α haloes: A pre-requisite for massive galaxy formation? I/2005A/2. – Mackey (IoA, Cambridge). A survey for dwarf galaxy remnants around outer halo globular clusters. I/2005A/1. – Ramsay (MSSL). RApid Time Survey — exploring a new temporal parameter space. I/2005A/3. – Zeilinger (Institute for Astronomy, Viena). Ages and metallicities of dwarf ellipticals in clusters at z=0.04. I/2005A/5.
60 • ING BIENNIAL R EPORT 2004–2005 NL PATT
– Aragon (Kapteyn Institute). Measuring galaxy spin alignments along a void-intersection filament near AWM3. i05an007. – Franx (Leiden Observatory). Practical astronomy for 2nd year students. i05an005. – Groot (Nijmegen). IPHAS — the INT/WFC photometric Hα survey of the northern galactic plane. i05an001. – Kovac (Kapteyn Institute). The optical counterparts of the smallest gas-rich galaxies. i05an006. – Röttgering (Sterrewacht Leiden). Ly-α emission line halos and the properties of z>2 proto-clusters. i05an002.
SP CAT
– Beckman (IAC). The links between bars and star formation: An advanced survey. I9/2005A. – Castro-Tirado (IAA-CSIC). Physical characterisation of Gamma-ray bursts (GRBs) in the SWIFT era. W25/2005A [sic]. – Deeg (IAC). Sample definition for exoplanet detection by the COROT spacecraft. I11/2005A. – Hatziminaoglou (IAC). Deep imaging in SWIRE ELAIS N1 and N2 fields. I1/2005A. – Iglesias (Laboratoire d'Astrophysique de Marseille). The impact of starbursts in the halos of dwarf galaxies. I6/2005A. – Leisy (IAC/ING). IPHAS — the INT/WFC photometric Hα survey of the northern galactic plane. I3/2005A. – López (IAC). The luminosity function of galaxies in Hercules supercluster. I10/2005A. – Martínez (Valencia). Dwarf galaxy population around isolated galaxies and in small groups. I4/2005A. – Martínez-Delgado (Max-Planck-Institut fur Astronomie, Heidelberg). Two new ultra-faint Milky Way companions. I13/2005A. – Zurita (Granada). Global morphology of star formation: Local calibration. I7/2005A.
Spanish Additional Time Allocations
– Rebolo (IAC/CSIC). Subestellar populations in young clusters and stellar associations: I. Orion Belt and Praesepe. I8/2005A. – Vílchez (IAA). Deep Hα imaging of clusters of galaxies in the WINGS Survey. I12/2005A.
SEMESTER 2005B
ITP Programmes on the ING Telescopes
– Peletier (Kapteyn), MAGPOP — The star formation history of dwarf galaxies, ITP4.
William Herschel Telescope
UK PATT
– Bosma (Observatoire de Marseille), Deep K-band surface photometry of low surface brightness galaxies. W/2005B/28. – Chappelle (Liverpool), The role of gravity upon ultracool dwarf dust formation. W/2005B/18. – Chrysostomou (Hertfordshire), Verifying the absence of jets from “misaligned” T-Tauris in the Taurus-Auriga molecular cloud. W/2005B/59. – Fender (Southampton), Echo-mapping a Quiescent Black Hole. W/2005B/75. – Hatch (IoA), Investigating the effects of the Perseus ICM on a supersonically infalling galaxy. W/2005B/38. – Hodgkin (IoA), Spectroscopy of Transit Candidates in the Orion and M34 Clusters. W/2005B/53. – Hough (Hertfordshire), PLANETPOL polarimetry of Upsilon Andromedae b. W/2005B/48. – Huxor (Hertfordshire), Metallicity and Radial Velocity Determinations of Newly Discovered M31 Halo Globular Clusters. W/2005B/52. – Jeffries (Keele), Binary statistics and the formation of low-mass stars and brown dwarfs. W/2005B/50. – Leigh (Liverpool), Spectroscopic detection and characterisation of the planet orbiting upsilon Andromeda. W/2005B/10. – Levan (Leicester), Probing the high redshift universe with GRBs. W/2005B/46. – Littlefair (Sheffield), J1702+3229 — a CV in the period gap with an evolved secondary. W/2005B/66. – Lucas (Hertfordshire), Determination of the primordial incidence of binarity in Orion Brown Dwarfs. W/2005B/55. – Marsh (Observatoire de Marseille), The nature of the white dwarfs in long period cataclysmic variables (CVs). W/2005B/32. – Nandra (ICL), The AGN luminosity function at z=3. W/2005B/26. – Napiwotzki (Leicester), Testing common envelope theory and SN Ia progenitor models with double white dwarfs. W/2005B/47. – Naylor (Exeter), Does star formation take a long time? W/2005B/67. – Nichol (Portsmouth), Spectroscopy of SNe Ia detected in the Sloan Digital Sky Survey II. W/2005B/19. – Oudmaijer (Leeds), NAOMI/OASIS observations of evolved cool supergiants: mirror, mirror on the wall. W/2005B/73. – Pollacco (QUB), Search for substellar companions to stars with extrasolar planets. W/2005B/23. – Pozzo (ICL), Late-time study of the very nearby Type IIP Supernova 2004dj. W/2005A/13. – Roques (Observatoire de Paris), Detection of small Kuiper Belt objects by stellar occultations. W/2005B/12. – Tanvir (Hertfordshire), The physics of short bursts and relativistic blast waves. W/2005B/25.
ING BIENNIAL R EPORT 2004–2005 • 61 NL PATT
– Aerts (Nijmegen), ULTRACAM asteroseismology: combining pressure and gravity modes to probe structure of BAL090100001. w05bn003. – Besselaar (Nijmegen), Follow-up of DB+dM binary systems. w05bn010. – Groot (Nijmegen), Optical-NIR Spectral eclipse mapping of accretion disks. w05bn014. – Jonker (SRON), Phase resolved photometry of the msec X-ray pulsar IGR J00291+5934 in quiescence. w05bn005. – McDermid (Leiden), Mapping the nuclear regions of early-type galaxies with OASIS. w05bn009. – Nelemans (Nijmegen), Testing common envelope theory and SN Ia progenitor models with double white dwarfs. w05bn008. – Nelemans (Nijmegen), Determining the accretion geometry and distance to the 10 min binary ES Cet. w05bn012. – Nelemans (Nijmegen), Fast photometry of the 10 min binary ES Cet with ULTRACAM. w05bn013. – Perez (Kapteyn), Origin of the very sub-solar hot gas abundances in X-ray low luminosity ellipticals. w05bn006. – Quirrenbach (Leiden), Line Bisector Variations for K Giants. w05bn007. – Roelofs (Nijmegen), Constraining the nature of the enigmatic variable V407 Vul. w05bn015. – Starling (Amsterdam), The physics of short bursts and relativistic blast waves. w05bn002. – Wijers (Amsterdam), Probing the high redshift universe with GRBs. w05bn001.
SP CAT
– Barrado (LAEFF), Membership of substellar candidates of the Collinder 69 and Barnard 35. WHT6/05B. – Beckman (IAC), Basic properties of nuclear bars in double bar galaxies. WHT15/05B. – Casares (IAC), Possible orbital period derivative in the black hole binary V404. WHT56/05B. – Casares (IAC), Determining system parameters of a Soft X-ray transient in outburst. WHT60/05B. – Castro-Tirado (IAA), GRB physics in the INTEGRAL and SWIFT era. WHT32-A/05B. – Elías de la Rosa (Observatorio di Padova), Detailed study of the physics of nearby Supernovae. WHT44-E/05B. – Erwin (IAC), The nature of bars in late-type spiral galaxies. WHT35/05B. – Erwin (IAC), How many galactic bulges are imposters? WHT55/05B. – García (IAC), 3D-spectroscopy of the Orion nebula. Local properties of the ionised gas associated with proplyds. WHT28/05B. – Gómez (IAC), Infrared characterisation of supernova progenitors. WHT13/05B. – González (CSIC), Finding an evolutionary link between radio galaxies and very luminous infrared galaxies. WHT3/05B. – Herrero (IAC), Luminous blue stars along the spiral arms of M33. WHT26/05B. – Kehrig (IAA), The problem of metal pollution in low metallicity HII-Galaxies. WHT27/05B. – López (IAC), Studying the origin of nuclear bars. WHT16/05B. – López (IAC), Star forming regions in starburst galaxies with tidal streams. WHT21/05B. – Martínez (IAA), Does M31 have as many satellites as predicted by Cold Dark Matter theory? WHT49/05B. – Negueruela (Alicante), A survey of blue stragglers in young open clusters. WHT58/05B. – Rodríguez (IAC), Unravelling the role of the SW Sextantis stars in the evolution of cataclysmic variables. WHT43-A/05B. – Rodríguez (IAC), The magnetic nature of the SW Sextantis stars. WHT48/05B. – Vázquez (IAC), Asteroseismology of the open cluster NGC7039. WHT23/05B.
Spanish Additional Time
– Acosta (IAC), Catalogue of infrared polarimetric standards of low luminosity. WHT47/05B. – Balcells (IAC), The GOYA survey. Photometric characterisation of high-z galaxies. WHT14/05B. – Bergond (IAA), Globular cluster populations of well defined isolated galaxies. WHT46/05B. – Hammersley (IAC), Visible spectroscopy of the GTC standards. WHT50/05B. – Manchado (IAC), LIRIS GT. – Martín (IAC), Preparation for GTC follow-up of brown dwarf candidates in young open clusters. WHT4-A/05B.
WHT–TNG Time Share
– Benn (ING), The nature of BAL outflows in quasars. T60. – Leone (OA Catania), Detecting magnetic fields in planetary nebulae, and understanding their role in the nebular shaping. T41. – Zaggia (OA Trieste), Hunting for cores of dwarf spheroidal galaxies in the external Milky Way Halo. T69.
Instrument Builders’ Guaranteed Time
– Bacon (Lyon). GT Type A. – Bacon (Lyon). GT Type B.
Isaac Newton Telescope
UK PATT
– Burleigh (Leicester), Faint planetary nebulae around hot white dwarfs. I/2005B/9.
62 • ING BIENNIAL R EPORT 2004–2005 – Drew (ICL), IPHAS — the INT/WFC photometric Hα survey of the Northern Galactic Plane. I/2005B/10. – Fender (Southampton), Jet-blown optical nebulae from black hole X-ray binaries. I/2005B/4. – Irwin (IoA), Searching for planetary transits in the Orion Nebula Cluster. I/2005B/17. – Irwin (IoA), A targeted CCD survey of the outer halo of M31. I/2005B/18. – Jarvis (Oxford), A wide-field search for Ly-α haloes: A pre-requisite for massive galaxy formation? I/2005B/2. – Littlefair (Exeter), How long do young stars remain locked to their discs? I/2005B/11. – Shanks (Durham), A UV survey to probe interactions between z~3 galaxies and the IGM. I/2005B/15. – Todd (QUB), The distance scale: eclipsing binaries and Cepheids in the dwarf irregular galaxy IC1613. I/2005B/8.
NL PATT
– Baes (ESO), Dust, dynamics and dark matter in elliptical galaxies — optical photometry. i05bn004. – Groot (Nijmegen), IPHAS — the INT/WFC photometric Hα survey of the Northern Galactic Plane. i05bn001. – Roelofs (Nijmegen), The HeI survey of the Galactic Plane: the AM CVn population. i05bn003. – Waters (Amsterdam), Search for faint Be stars in the COROT fields. i05bn002.
SP CAT
– Alonso (IAC), The search for hot Neptunes using the field star transit method. INT3/05B. – Castro-Tirado (IAA), The physics of GRBs in the INTEGRAL and SWIFT era. INT11/05B. – da Rocha (Göttingen), Intra-group light in Hickson compact groups. INT5/05B. – Deeg (IAC), Sample definition for exoplanet detection by the COROT spacecraft. INT9/05B. – López (IAC), Quantitative morphology of galaxies in nearby clusters. INT6/05B. – Mampaso (IAC), IPHAS — the INT/WFC photometric Hα survey of the Northern Galactic Plane. INT3/05B. – Morales (LAEFF), Exploring the different initial mass functions in the l Orionis SFR. INT1/05B. – Rosenberg (IAC), The formation and evolution of the Milky Way (III): the Galactic disc. INT4/05B.
Spanish Additional Time Allocations
– Herrero (IAC), Detecting the blue massive star population to 5 Mpc for OSIRIS. INT10/05B. – Ruiz (Barcelona), Supernovae at z=0.05–0.35: studying the nature of the dark energy (II). INT15/05B. – Vílchez (IAA), Deep Hα imaging of clusters of galaxies in the WINGS survey. INT14/05B.
ING BIENNIAL R EPORT 2004–2005 • 63 Appendix E
ING BIBLIOGRAPHY
Below is the list of research papers published in 2004 and 2005 that resulted from observations carried out at the telescopes of the Isaac Newton Group. The data used in these papers was obtained as part of an observing programme or by mining one of the ING archives. The selection process identifies papers that make direct use of observations obtained with the ING telescopes, in order to qualify. Papers that refer to data presented in earlier papers (derivative papers) are not counted. This bibliography was compiled from only the refereed journals MNRAS, Astrophys J, Astrophys J Letters, Astrophys J Suppl, Astron J, PASP, Astron Astrophys, Nature and Science, although many other publications have appeared elsewhere, notably in workshop, conference proceedings and PhD theses. For every paper the following information is given: author/s, title, journal, volume, first page, nationality of the first institution of the first author (between brackets), used instrument (between parentheses) and the ING Archive as the data source or Service if obtained on a service night when this was credited in the paper.
2004
WILLIAM HERSCHEL TELESCOPE
1. B. Acke, C. Waelkens, "Chemical analysis of 24 dusty (pre-)main-sequence stars", Astron Astrophys, 427, 1009. [BELGIUM] (UES) 2. A. Afonso-Luis, E. Hatziminaoglou, I. Pérez-Fournon, E. A. González-Solares, M. Rowan-Robinson, M. Vaccari, C. Lari, S. Serjeant, S. Oliver, A. Hernán-Caballero, F. M. Montenegro-Montes, "A study of the 15-µm quasars in the ELAIS N1 and N2 fields", MNRAS, 354, 961. [SP] (AF2) 3. A. Ahmad, C. S. Jeffery, A. W. Fullerton, "Discovery of a spectroscopic binary comprising two hot helium-rich subdwarfs", Astron Astrophys, 418, 275. [UK] (ISIS) 4. M. E. van den Ancker, P. F. C. Blondel, H. R. E. Tjin A Djie, K. N. Grankin, O. V. Ezhkova, V. S. Shevchenko, E. Guenther, B. Acke, "The stellar composition of the star formation region CMa R1 — III. A new outburst of the Be star component in Z CMa", MNRAS, 349, 1516. [GERMANY] (UES) 5. H. Arp, C. M. Gutiérrez, M. López-Corredoira, "New optical spectra and general discussion on the nature of ULXs", Astron Astrophys, 418, 877. [GERMANY] (ISIS) 6. T. S. R. Babbedge, M. Rowan-Robinson, E. Gonzalez-Solares, M. Polletta, S. Berta, I. Pérez-Fournon, S. Oliver, D. M. Salaman, M. Irwin, S. J. Weatherley, "ImpZ: a new photometric redshift code for galaxies and quasars", MNRAS, 353, 654. [UK] (AF2) 7. D. Baines, R. D. Oudmaijer, A. Mora, C. Eiroa, John M. Porter, B. Merín, B. Montesinos, D. de Winter, A. Cameron, J. K. Davies, H. J. Deeg, R. Ferlet, C. A. Grady, A. W. Harris, M. G. Hoare, K. Horne, S. L. Lumsden, L. F. Miranda, A. Penny, A. Quirrenbach, "The pre-main-sequence binary HK Ori: spectro-astrometry and EXPORT data", MNRAS, 353, 697. [UK] (UES) 8. G. Bihain, G. Israelian, R. Rebolo, P. Bonifacio, P. Molaro, "Cu and Zn in the early Galaxy", Astron Astrophys, 423, 777. [SP] (UES) 9. D. L. Block, R. Buta, J. H.Knapen, D. M. Elmegreen, B. G. Elmegreen, I.Puerari, "Gravitational Bar And Spiral Arm Torques From Ks-Band Observations And Implications For The Pattern Speeds", Astron J, 128, 183. [SOUTH AFRICA] (INGRID) 10. V. Botte, S. Ciroi, P. Rafanelli, F. Di Mille, "Exploring Narrow-Line Seyfert 1 Galaxies Through The Physical Properties Of Their Hosts", Astron J, 127, 3168. [ITALY] (ISIS+ARCHIVE) 11. R. G. Bower, S. L. Morris, R. Bacon, R. J. Wilman, M. Sullivan, S. Chapman, R. L. Davies, P. T. de Zeeuw, E. Emsellem, "Deep SAURON spectral imaging of the diffuse Lyman α halo LAB1 in SSA 22", MNRAS, 351, 63. [UK] (SAURON) 12. F. J. Carrera, M. J. Page, J. P. D. Mittaz, "XMM-Newton spectra of hard spectrum Rosat AGN: X-ray absorption and optical reddening", Astron Astrophys, 420, 163. [SP] (ISIS) 13. J. M. Castro Cerón, J. Gorosabel, A. J. Castro-Tirado, V. V. Sokolov, V. L. Afanasiev, T. A. Fatkhullin, S. N. Dodonov, V. N. Komarova, A. M. Cherepashchuk, K. A. Postnov, U. Lisenfeld, J. Greiner, S. Klose, J. Hjorth, J. P. U. Fynbo, H. Pedersen, E. Rol, J. Fliri, M. Feldt, G. Feulner, M. I. Andersen, B. L. Jensen, M. D. Pérez Ramírez, F. J. Vrba, A. A. Henden, G. Israelian, N. R. Tanvir, "On the constraining observations of the dark GRB 001109 and the properties of a z = 0.398 radio selected starburst galaxy contained in its error box", Astron Astrophys, 424, 833. [SP] (INGRID, PFIP)
64 • ING BIENNIAL R EPORT 2004–2005 14. A. J. Cenarro, P. Sánchez-Blázquez, N. Cardiel, J. Gorgas, "Early-Type Galaxies in the Coma Cluster: A New Piece in the Calcium Puzzle", Astrophys J, 614, L101. [SP] (ISIS) 15. N. N. Chugai, S. I. Blinnikov, R. J. Cumming, P. Lundqvist, A. Bragaglia, A. V. Filippenko, D. C. Leonard, T.Matheson, J.Sollerman, "The Type IIn supernova 1994W: evidence for the explosive ejection of a circumstellar envelope", MNRAS, 352, 1213. [RUSSIA] (ISIS) 16. L. Clewley, S. J. Warren, P. C. Hewett, J. E. Norris, N. W. Evans, "Distant field blue horizontal branch stars and the mass of the Galaxy — II. Photometry and spectroscopy of UKST candidates 16 < B < 19.5, 11 < R < 52 kpc", MNRAS, 352, 285. [UK] (ISIS) 17. L. Colina,S. Arribas,D. Clements, "INTEGRAL Field Spectroscopy of the Extended Ionized Gas in Arp 2201", Astrophys J, 602, 181. [SP] (INTEGRAL) 18. Y. Copin, N. Cretton, E. Emsellem, "Axisymmetric dynamical models for SAURON and OASIS observations of NGC 3377", Astron Astrophys, 415, 889. [FRANCE] (SAURON) 19. P. C. Dawson, M. M. De Robertis, "Barnard's Star And The M Dwarf Temperature Scale", Astron J, 127, 2909. [CANADA] (ISIS+ARCHIVE) 20 .A. J. Delgado, L. F. Miranda, M. Fernández, E. J. Alfaro, "Photometric And Spectroscopic Study Of Stars In The Field Of The Young Open Cluster Roslund 4", Astron J, 128, 330. [SP] (ISIS) 21. P. D. Dobbie, D. J. Pinfield, R. Napiwotzki, N. C. Hambly, M. R. Burleigh, M. A. Barstow, R. Jameson, F. Jameson, I. Hubeny, "Praesepe and the seven white dwarfs", MNRAS, 355, L39. [UK] (ISIS) 22. M. Doherty, A. Bunker, R. Sharp, G. Dalton, I. Parry, I. Lewis, E. MacDonald, C. Wolf, H. Hippelein, "Multi-object near-infrared Hα spectroscopy of z~1 star-forming galaxies in the Hubble Deep Field North", MNRAS, 354, L7. [UK] (CIRPASS) 23. I. Domínguez, C. Abia, O. Straniero, S. Cristallo, Ya. V. Pavlenko, "First detection of a lithium rich carbon star in the Draco dwarf galaxy: Evidence for a young stellar population", Astron Astrophys, 422, 1045. [SP] (ISIS) 24. J. E. Drew, M. J. Barlow, Y. C. Unruh, Q. A. Parker, R. Wesson, M. J. Pierce, M. R. W. Masheder, S. Phillipps, "Discovery of a WO star in the Scutum-Crux arm of the inner Galaxy", MNRAS, 351, 206. [UK] (ISIS) 25. A. Ecuvillon, G. Israelian, N. C. Santos, M. Mayor, R. J. García López, S. Randich, "Nitrogen abundances in planet-harbouring stars", Astron Astrophys, 418, 703. [SP] (UES) 26. S. L. Ellison, C.W. Churchill, S. A. Rix, M. Pettini, "The Number Density of 0.6 ING BIENNIAL R EPORT 2004–2005 • 65 42. R. I. Hynes, P. A. Charles, M. R. Garcia, E. L. Robinson, J. Casares, C. A. Haswell, A. K. H. Kong, M. Rupen, R. P. Fender, R. M. Wagner, E. Gallo, B. A. C. Eves, T. Shahbaz, C. Zurita, "Correlated X-Ray and Optical Variability in V404 Cygni in Quiescence", Astrophys J, 611, L125. [USA] (ISIS) 43. R. I. Hynes, P. A. 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Dennefeld, "Planetary nebulae in the dwarf galaxy NGC 6822: Detection of new candidates", Astron Astrophys, 436, 437. [SP] (WFC) 47. R. López, R. Estalella, A. C. Raga, A. Riera, B. Reipurth, S. R. Heathcote, "3-D kinematics of the HH 110 jet", Astron Astrophys, 432, 567. [SP] (PFIP) 48. L. Magrini, R. L. M. Corradi, R. Greimel, P. Leisy, A. Mampaso, M. Perinotto, J. R. Walsh, N. A. Walton, A. A. Zijlstra, D. Minniti, M. Mora, "The Local Group Census: searching for planetary nebulae in IC 1613, WLM and GR8", MNRAS, 361, 517. [ITALY] (WFC) 49. E. L. Martín, A. Magazzù, X. Delfosse, R. D. Mathieu, "The pre-main sequence spectroscopic binary UZ Tau East: Improved orbital parameters and accretion phase dependence", Astron Astrophys, 429, 939. [SP] (IDS) 50. E. L. Martín, A. Magazzù, R. J. García López, S. Randich, D. Barrado y Navascués, "On the potassium-rotation connection in late-type Alpha Persei stars", Astron Astrophys, 429, 1051. [SP] (IDS) 76 • ING BIENNIAL R EPORT 2004–2005 51. A. Matkovic, R. Guzmán, "Kinematic properties and stellar populations of faint early-type galaxies — I. Velocity dispersion measurements of central Coma galaxies", MNRAS, 362, 289. [USA] (WFC) 52. R. Minchin, J. Davies, M. Disney, P. Boyce, D. Garcia, C. Jordan, V. Kilborn, R. Lang, S. Roberts, S. Sabatini, W. van Driel, "A Dark Hydrogen Cloud in the Virgo Cluster", Astrophys J, 622, L21. [UK] (WFC) 53. L. Morales-Rueda, T. R. Marsh, P. F. L. Maxted, G. Nelemans, C. Karl, R. Napiwotzki, C. K. J. Moran, "Six detached white-dwarf close binaries", MNRAS, 359, 648. [NL] (IDS) 54. T. Naylor, A. Allan, K. S. Long, "The masses, radii and luminosities of the components of U Geminorum", MNRAS, 361, 1091. [UK] (IDS) 55. S. G. Neff et al., "Ultraviolet Emission from Stellar Populations within Tidal Tails: Catching the Youngest Galaxies in Formation?", Astrophys J, 619, L91. [USA] (WFC+ARCHIVE) 56. G. Nelemans, R. Napiwotzki, C. Karl, T. R. Marsh, B. Voss, G. Roelofs, R. G. Izzard, M. Montgomery, T. Reerink, N. Christlieb, D. Reimers, "Binaries discovered by the SPY project", Astron Astrophys, 440, 1087. [NL] (IDS) 57. M. B. Pracy, S. P. Driver, R. De Propris, W. J. Couch, P. E. J. Nulsen, "Luminosity segregation in three clusters of galaxies (A119, A2443, A2218)", MNRAS, 364, 1147. [AUSTRALIA] (WFC) 58. G. Ramsay, P. Hakala, "RApid Temporal Survey (RATS) — I. Overview and first results", MNRAS, 360, 314. [UK] (WFC) 59. P. Reig, I. Negueruela, G. Papamastorakis, A. Manousakis, T. Kougentakis, "Identification of the optical counterparts of high-mass X-ray binaries through optical photometry and spectroscopy", Astron Astrophys, 440, 637. [GREECE] (IDS) 60. I. Ribas, C. Jordi, F. Vilardell, E. L. Fitzpatrick, R. W. Hilditch, E. F. Guinan, "First Determination of the Distance and Fundamental Properties of an Eclipsing Binary in the Andromeda Galaxy", Astrophys J, 635, L37. [SP] (WFC) 61. G. Rodighiero, D. Fadda, A. Franceschini, C. Lari, "A far-infrared view of the Lockman hole from ISO 95-µm observations — II. Optical identifications and insights into the nature of the far-infrared sources", MNRAS, 357, 449. [ITALY] (WFC) 62. M. Rowan-Robinson, T. Babbedge, J. Surace, D. Shupe, F. Fang, C. Lonsdale, G. Smith, M. Polletta, B. Siana, E. González-Solares, K. Xu, F. Owen, P. Davoodi, H. Dole, D. Domingue,A. Efstathiou, D. Farrah, M. Fox, A. Franceschini, D. Frayer, E. Hatziminaoglou, F. Masci, G.Morrison, K. Nandra, S.Oliver, N. Onyett, D. Padgett, I. Pérez-Fournon, S. Serjeant, G. Stacey, M. Vaccari, "Spectral Energy Distributions And Luminosities Of Galaxies And Active Galactic Nuclei In The Spitzer Wide-Area Infrared Extragalactic (Swire) Legacy Survey", Astron J, 129, 1183. [UK] (WFC) 63. S. Sabatini, J. Davies, W. van Driel, M. Baes, S. Roberts, R. Smith, S. Linder, K. O'Neil, "The dwarf low surface brightness galaxy population of the Virgo Cluster — II. Colours and HI line observations", MNRAS, 357, 819. [UK] (WFC) 64. R. Sánchez-Janssen, J. Iglesias-Páramo, C. Muñoz-Tuñón, J. A. L. Aguerri, J. M. Vílchez, "The V-band luminosity function of galaxies in A2151", Astron Astrophys, 434, 521. [SP] (WFC) 65. J. E. Skelton, A. Lawrence, A. Pappa, P. Lira, O. Almaini, "Short time-scale optical variability of the dwarf Seyfert nucleus in NGC 4395", MNRAS, 358, 781. [UK] (IDS) 66. R. C. Smith, O. Mehes, D. Vande Putte, N. A. Hawkins, "A non-main-sequence secondary in SY Cancri", MNRAS, 360, 364. [UK] (IDS) 67. J. Southworth, B. Smalley, P. F. L. Maxted, A. Claret, P. B. Etzel, "Absolute dimensions of detached eclipsing binaries — I. The metallic-lined system WW Aurigae", MNRAS, 363, 529. [UK] (IDS) 68. P. B. Stetson, "Homogeneous Photometry. IV. On The Standard Sequence In The Globular Cluster Ngc 2419", PASP, 117, 563. [CANADA] (PFIP+ARCHIVE) 69. P. B. Stetson, M. Catelan, H. A. Smith, "Homogeneous Photometry. V. The Globular Cluster Ngc 4147", PASP, 117, 1325. [CANADA] ((PFIP, JKT CCD)+ARCHIVE) 70. R. A. Street, Keith Horne, T. A. Lister, A. Penny, Y. Tsapras, A. Quirrenbach, N. Safizadeh, J. Cooke, D. Mitchell, A. Collier Cameron, "Variable stars in the field of open cluster NGC 6819 — II", MNRAS, 358, 795. [UK] (WFC) 71. G. Tagliaferri, L. A. Antonelli, G. Chincarini, A. Fernández-Soto, D. Malesani, M. Della Valle, P. D'Avanzo, A. Grazian, V. Testa, S. Campana, S. Covino, F. Fiore, L. Stella, A. J. Castro-Tirado, J. Gorosabel, D. N. Burrows, M. Capalbi, G. Cusumano, M. L. Conciatore, V. D'Elia, P. Filliatre, D. Fugazza, N. Gehrels, P. Goldoni, D. Guetta, S. Guziy, E. V. Held, K. Hurley, G. L. Israel, M. Jelínek, D. Lazzati, A. López-Echarri, A. Melandri, I. F. Mirabel, M. Moles, A. Moretti, K. O. Mason, J. Nousek, J. Osborne, L. J. Pellizza, R. Perna, S. Piranomonte, L. Piro, A. de Ugarte Postigo, P. Romano, "GRB 050904 at redshift 6.3: observations of the oldest cosmic explosion after the Big Bang", Astron Astrophys, 443, L1. [ITALY] (WFC) 72. E. L. Taylor, R. G. Mann, A. N. Efstathiou, T. S. R. Babbedge, M. Rowan-Robinson, G. Lagache, A. Lawrence, S. Mei, M. Vaccari, Ph. Héraudeau, S. J. Oliver, M. Dennefeld, I. Perez-Fournon, S. Serjeant, E. González-Solares, J.-L. Puget, H. Dole, C. Lari, "Properties of FIRBACK-ELAIS 175-µm sources in the ELAIS N2 region", MNRAS, 361, 1352. [UK] (WFC) 73. The Tempel 1 Observing Collaborators Team, "Deep Impact: Observations from a Worldwide Earth-based Campaign", Science, 310, 265. [USA] (LIRIS, WFC) 74. I. Todd, D. Pollacco, I. Skillen, D. M. Bramich, S. Bell, T. Augusteijn, "A survey of eclipsing binary stars in the eastern spiral arm of M31", MNRAS, 362, 1006. [UK] (WFC, ARCHIVE) 75. D. A. Wake, C. A. Collins, R. C. Nichol, L. R. Jones, D. J. Burke, "The Environmental Dependence of Galaxy Colors in Intermediate-Redshift X-Ray-selected Clusters", Astrophys J, 627, 186. [UK] (WFC) 76. K. Weis, D. J. Bomans, "SN 2002kg — the brightening of LBV V37 in NGC 2403", Astron Astrophys, 429, L13. [GERMANY] ((PFIP+JKT CCD)+ARCHIVE) ING BIENNIAL R EPORT 2004–2005 • 77 77. R. Wesson, X-W. Liu, M. J. Barlow, "The abundance discrepancy–recombination line versus forbidden line abundances for a northern sample of galactic planetary nebulae", MNRAS, 362, 424. [UK] (IDS) 78. B. Willman, J. J. Dalcanton, D. Martínez-Delgado, A. A. West, M. R. Blanton, D. W. Hogg, J. C. Barentine, H. J. Brewington, M. Harvanek, S. J. Kleinman, J. Krzesinski, D. Long, E. H. Neilsen, Neilsen, Jr., A. Nitta, S. A. Snedden, "A New Milky Way Dwarf Galaxy in Ursa Major", Astrophys J, 626, L85. [USA] (WFC) 79. S. A. Wright, R .L. M. Corradi, M. Perinotto, "Absolute spectrophotometry of northern compact planetary nebulae", Astron Astrophys, 436, 967. [SP] (IDS, WFC) 80. P. Zhao, J. E. Grindlay, J. Sub Hong, S. Laycock, X. P. Koenig, E. M. Schlegel, M. van den Berg, "ChaMPlane Optical Survey: Mosaic Photometry", Astrophys J Suppl, 161, 429. [USA] (WFC) JACOBUS KAPTEYN TELESCOPE 1. J. A. L. Aguerri, N. Elias-Rosa, E. M. Corsini, C. Muñoz-Tuñón, "Photometric properties and origin of bulges in SB0 galaxies", Astron Astrophys, 434, 109. [SP] (JKT CCD) 2. L. Balaguer-Núñez, C. Jordi, D. Galadí-Enríquez, "uvby Hβ CCD photometry and membership segregation of the open cluster NGC 2548; gaps in the Main Sequence of open clusters", Astron Astrophys, 437, 457. [SP] (JAG CCD) 3. R. Barrena, M. Ramella, W. Boschin, M. Nonino, A. Biviano, E. Mediavilla, "VGCF detection of galaxy systems at intermediate redshifts", Astron Astrophys, 444, 685. [SP] (JKT CCD) 4. C. S. Brinkworth, T. R. Marsh, L. Morales-Rueda, P. F. L. Maxted, M. R. Burleigh, S. A. Good, "Rotational period of WD 1953-011 — a magnetic white dwarf with a star-spot", MNRAS, 357, 333. [UK] (JAG CCD) 5. P. Erwin, "How large are the bars in barred galaxies?", MNRAS, 364, 283. [SP] (JKT CCD+ARCHIVE) 6. K. M. Exter, D. L. Pollacco, P. F. L. Maxted, R. Napiwotzki, S. A. Bell, "A study of two post-common envelope binary systems", MNRAS, 359, 315. [UK] (JKT CCD) 7. B. T. Gänsicke, T. R. Marsh, A. Edge, P. Rodríguez-Gil, D. Steeghs, S. Araujo-Betancor, E. Harlaftis, O. Giannakis, S. Pyrzas, L. Morales- Rueda, A. Aungwerojwit, "Cataclysmic variables from a ROSAT/2MASS selection — I. Four new intermediate polars", MNRAS, 361, 141. [UK] (ISIS, IDS, JKT CCD) 8. M. A. Hendry, S. J. Smartt, J. R. Maund, A. Pastorello, L. Zampieri, S. Benetti, M. Turatto, E. Cappellaro, W. P. S. Meikle, R. Kotak, M. J. Irwin, P. G. Jonker, L. Vermaas, R. F. Peletier, H. van Woerden, K. M. Exter, D. L. Pollacco, S. Leon, S. Verley, C. R. Benn, G. Pignata, "A study of the Type II-P supernova 2003gd in M74", MNRAS, 359, 906. [UK] (WFC, JKT CCD) 9. P. A. James, N. S. Shane, J. H. Knapen, J. Etherton, S. M. Percival, "The Hα Galaxy Survey", Astron Astrophys, 429, 851. [UK] (JAG CCD+SERVICE) 10. L. Jamet, G. Stasinska, E. Pérez, R. M. González Delgado, J. M. Vílchez, "What is the temperature structure in the giant HII region NGC 588?", Astron Astrophys, 444, 723. [FRANCE] (JKT CCD+ARCHIVE) 11. J. H. Knapen, "Structure and star formation in disk galaxies. III. Nuclear and circumnuclear Hα emission", Astron Astrophys, 429, 141. [UK] (PFIP, WFC, WFC+ARCHIVE, JAG CCD, JKT CCD+SERVICE, JAG CCD+ARCHIVE) 12. S. P. Littlefair, T. Naylor, B. Burningham, R. D. Jeffries, "Do accretion discs regulate the rotation of young stars?", MNRAS, 358, 341. [UK] (JKT CCD) 13. P. Reig, I. J. Fabregat, R. Chato, M. J. Coe, "Long-term optical/IR variability of the Be/X-ray binary LS V +44 17/RX J0440.9+4431", Astron Astrophys, 440, 1079. [GREECE] (JKT CCD) 14. M. Relaño, J. E. Beckman, A. Zurita, M. Rozas, C. Giammanco, "The internal dynamical equilibrium of H II regions: A statistical study", Astron Astrophys, 431, 235. [SP] (JKT CCD) 15. P. Rodríguez-Gil, B. T. Gänsicke, H.-J. Hagen, D. Nogami, M. A. P. Torres, H. Lehto, A. Aungwerojwit, S. Littlefair, S. Araujo-Betancor, D. Engels, "HS 0943+1404, a true intermediate polar", Astron Astrophys, 440, 701. [UK] (JKT CCD) 16. R. C. Smith, O. Mehes, D. V. Putte, N. A. Hawkins, "A non-main-sequence secondary in SY Cancri", MNRAS, 360, 364. [UK] (JKT CCD) 17. P. B. Stetson, M. Catelan, H. A. Smith, "Homogeneous Photometry. V. The Globular Cluster NGC 41471", PASP, 117, 1325. [CANADA] ((PFIP, JAG CCD)+ARCHIVE)) 18. K. Weis, D. J. Bomans, "SN 2002kg — the brightening of LBV V37 in NGC 2403", Astron Astrophys, 429, L13. [GERMANY] (JKT CCD+ARCHIVE) 78 • ING BIENNIAL R EPORT 2004–2005 Appendix F ASTRONOMY STAFF RESEARCH PUBLICATIONS The following includes all 102 refereed and non-refereed publications of ING astronomers in the year 2004 (50 refereed journal papers and 52 non-refereed papers in conference proceedings or other publications), and all 84 refereed and non- refereed publications in the year 2005 (37 refereed journal papers and 47 non-refereed papers in conference proceedings or other publications). It is sorted by year and in alphabetical order (ING author appears in italic and bold). 2004 1. Ahmad, A., Jeffery, C. S., Solheim, J.-E., Østensen, R., “Pulsation stability of helium-rich subdwarf B stars”, Astrophys J Suppl, 291, 435. 2. Azzaro, M., Prada, F., Gutiérrez, C. M., “Motion Properties of Satellites around External Spiral Galaxies”, ASP Conf Series, 327, 268. 3. Benetti, S., Meikle, P., Stehle, M., Altavilla, G., Desidera, S., Folatelli, G., Goobar, A., Mattila, S., Méndez, J., Navasardyan, H., Pastorello, A., Patat, F., Riello, M., Ruiz-Lapuente, P., Tsvetkov, D., Turatto, M., Mazzali, P., Hillebrandt, W., “Supernova 2002bo: inadequacy of the single parameter description”, MNRAS, 348, 261. 4. Benn, C. R., Blanken, M., Bevil, C., Els, S., Goodsell, S., Gregory, T., Jolley, P., Longmore, A. J., Martin, O., Myers, R. M., Østensen, R., Rees, S., Rutten, R. G. M., Söchting, I., Talbot, G., Tulloch, S. M., “NAOMI: adaptive optics at the WHT”, Proc SPIE, 5490, 79. 5. Binzel, R. P., Licandro, J., Serra-Ricart, M., de León Cruz, J., Pinilla-Alonso, N., “Comet C/2003 WT_42 (LINEAR)”, IAU Circ, 8270, 1. 6. Bond, H. E., Henden, A., Levay, Z. G., Panagia, N., Sparks, W. B., Starrfield, S., Wagner, R. M., Corradi, R. L. M., Munari, U., “Hubble Space Telescope Observations of the Light Echoes around V838 Monocerotis”, ASP Conf Ser, 313, 543. 7. Carpano, S., Wilms, J., Schirmer, M., Kendziorra, E., “X-Ray properties of NGC 300 point sources detected with XMM-Newton, and their optical counterparts”, Mem Soc Astron Ital, 75, 486. 8. Clarkson, W. I., Christian, D. C., Collier-Cameron, A., Evans, N., Fitzsimmons, A., Haswell, C. A., Hellier, C., Hodgkin, S. T., Horne, K. D., Kane, S. R., Keenan, F. P., Lister, T. A., Norton, A. J., Pollacco, D. L., Ryans, R., Skillen, I., Street, R. A., West, R. G., Wheatley, P. J., “Current Status of the SuperWASP Project, American Astronomical Society Meeting Abstracts, 205. 9. Corradi, R. L. M., “Planetary Nebulae Morphology According to Padre Angelo Secchi”, ASP Conf Ser, 313, 25. 10. Corradi, R. L. M., “Multiple, Coeval and Hubble-Like Bipolar Outflows”, ASP Conf Ser, 313, 148. 11. Corradi, R. L. M., “Discussion Session on Nebulae Around Symbiotic Stars”, ASP Conf Ser, 313, 558. 12. Corradi, R. L. M., “The Bull's Eye Pattern in the Cat's Eye and Other Planetary Nebulae”, ING Newsl, 8, 10. 13. Corradi, R. L. M., Sánchez-Blázquez, P., Giammanco, C., Mellema, G., Schwarz, H. E., “New Rings in Planetary Nebulae Haloes”, ASP Conf Ser, 313, 290. 14. Corradi, R. L. M., Sánchez-Blázquez, P., Mellema, G., Giammanco, C., Schwarz, H. E., “Rings in the haloes of planetary nebulae”, Astron Astrophys, 417, 637. 15. Corradi, R. L. M., “Stellar paleontology using planetary nebulae”, Mem Soc Astron Ital, 75, 73. 16. Crowther, P. A., Evans, C. J., “CNO Abundances in Magellanic Cloud OB Supergiants”, IAU Symposium, 215, 218. 17. de León, J., Duffard, R., Licandro, J., Lazzaro, D., “Mineralogical characterization of A-type asteroid (1951) Lick”, Astron Astrophys, 422, L59. 18. Dotto, E., Fornasier, S., Barucci, M. A., Boehnhardt, H., Hainaut, O., Marzari, F., Licandro, J., de Bergh, C., “Visible and near-infrared spectroscopic survey of Jupiter Trojan asteroids: investigation of dynamical families”, AAS/Division for Planetary Sciences Meeting Abstracts, 36. 19. Duffard, René; Lazzaro, Daniela; Licandro, Javier; de Sanctis, Maria Cristina; Capria, Maria Teresa; Carvano, Jorge M., “Mineralogical characterization of some basaltic asteroids in the neighborhood of (4) Vesta: first results”, Icarus, 171, 120. 20. Ellison, S. L., Churchill, C. W., Rix, S. A., Pettini, M., “The Number Density of 0.6 ING BIENNIAL R EPORT 2004–2005 • 79 23. Evans, C. J., Lennon, D. J., Trundle, C., Heap, S. R., Lindler, D. J., “Terminal Velocities of Luminous, Early-Type Stars in the Small Magellanic Cloud”, Astrophys J, 607, 451. 24. Evans, C. J., Lennon, D. J., Walborn, N. R., Trundle, C., Rix, S. A., “The Ultraviolet and Optical Spectra of Luminous B-Type Stars in the Small Magellanic Cloud”, PASP, 116, 909. 25. Evans, C. J., Howarth, I. D., Irwin, M. J., Burnley, A. W., Harries, T. J., “A 2dF survey of the Small Magellanic Cloud”, MNRAS, 353, 601. 26. Fadeyev, V., et al., including Méndez, J., “Cosmological Constraints from the First Supernova Discovered above Redshift of One”, American Astronomical Society Meeting Abstracts, 205. 27. Flix, J., Martínez, M., Prada, F., The MAGIC Collaboration, “Indirect Searches for SUSY Dark Matter with the MAGIC Cherenkov Telescope”, ASP Conf Ser, 327, 47. 28. Funes, J. G., Gutiérrez, C. M., Prada, F., Azzaro, M., Ribeiro, M. B., “Star Formation in Satellite Galaxies”, ASP Conf Ser, 327, 272. 29. Gabasch, A., Salvato, M., Saglia, R. P., Bender, R., Hopp, U., Seitz, Feulner, G., Pannella, M., Drory, N., Schirmer, M., Erben, T., “The Star Formation Rate History in the FORS Deep and GOODS-South Fields”, Astrophys J, 616, L83. 30. Garavini, G., et al. (with Méndez, J.), “Spectroscopic Observations and Analysis of the Peculiar SN 1999aa”, Astron J, 128, 387. 31. Giavalisco, M., et al. (with Schirmer, M.) 2004, “The Great Observatories Origins Deep Survey: Initial Results from Optical and Near-Infrared Imaging”, Astrophys J, 600, L93. 32. Gonçalves, D. R., Mampaso, A., Corradi, R. L. M., Perinotto, M., “The Physical Parameters and Excitation of Jets and Knots in PNe”, ASP Conf Ser, 313, 198. 33. Groot, P.J., Rutten, R.G.M., van Paradijs, J., “A spectrophotometric study of RW Trianguli”, Astron Astrophys, 417, 333. 34. Gonçalves, D. R., Mampaso, A., Corradi, R. L. M., Perinotto, M., Riera, A., López-Martín, L., “K 4-47: a planetary nebula excited by photons and shocks”, MNRAS, 355, 37. 35. Gonçalves, D. R., Corradi, R. L. M., Mampaso, A., Perinotto, M., Erratum: ``The Physical Parameters, Excitation, and Chemistry of the Rim, Jets, and Knots of the Planetary Nebula NGC 7009'', Astrophys J, 601, 1161. 36. 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Licandro, J., “The Deep Impact Event as Seen from the Roque de Los Muchachos Observatory”, ING Newsl, 10, 4. 50. Licandro, J., Pinilla-Alonso, N., “The Inhomogeneous Surface of Centaur 32522 Thereus (2001 PT13)”, Astrophys J, 630, L93. 51. Magrini, L., Corradi, R. L. M., Greimel, R., Leisy, P., Mampaso, A., Perinotto, M., Walsh, J. R., Walton, N. A., Zijlstra, A. A., Minniti, D., Mora, M., “The Local Group Census: searching for planetary nebulae in IC 1613, WLM and GR8”, MNRAS, 361, 517. 52. Magrini, L., Leisy, P., Corradi, R. L. M., Perinotto, M., Mampaso, A., Vílchez, J. M., ”The chemistry of planetary nebulae and HII regions in the dwarf galaxies Sextans A and B from deep VLT spectra”, Astron Astrophys, 443, 115. 53. Mampaso, A., Corradi, R. L. M., “Imaging resources for the GTC: IPHAS”, Rev Mex Astron Astrof Conf Ser, 24, 52. 54. Mattila, S., Greimel, R., Gerardy, C., Meikle, W. P. S 2005, “Supernova 2005V in NGC 2146”, IAU Circ, 8474, 1. 55. Mattila, S., Greimel, R., Gerardy, C., Meikle, W. P. S., Clements, D. L., Nandra, K., “Arp 299”, IAU Circ, 8477, 2. 56. Mattila, S., Greimel, R., Gerardy, C., Meikle, W. P. S., Monard, L. A. G., Boles, T., Pugh, H., Graham, J., Li, W., “Supernovae 2005Q, 2005R, 2005S, 2005T, 2005U”, IAU Circ, 8473, 1. 57. Mattila, S., Greimel, R., Meikle, P., “LIRIS Discovers Supernovae in Starburst Galaxies”, ING Newsl, 9, 16. 58. Mazzali, P. A., et al. (with Méndez, J.), 2005, “High-Velocity Features: A Ubiquitous Property of Type Ia Supernovae”, Astrophys J, 623, L37. 59. Meech, K. J., et al., “Deep Impact: Observations from a Worldwide Earth-Based Campaign”, Science, 310, 265. 60. Méndez, J., “The Search for the Companion Star of Tycho Brahe's 1572 Supernova”, ING Newsl, 9, 20. 61. Méndez, J., Ruiz-Lapuente, P., Altavilla, G., Balastegui, A., Irwin, M., Schamanache, K., Balland, C., Pain, R., Walton, N., “Supernova Search at Intermediate-redshift. II. Host Galaxy Morphology”, ASP Conf Ser, 342, 488. 62. Munari, U., Henden, A., Vallenari, A., Bond, H. E., Corradi, R. L. M., Crause, L., Desidera, S., Giro, E., Marrese, P. M., Ragaini, S., Siviero, A., Sordo, R., Starrfield, S., Tomov, T., Villanova, S., Zwitter, T., Wagner, R. M., “UBV(RI)c photometry of stars around V838 Mon (Munari+, 2005)”, VizieR Online Data Catalog, 343, 41107. 63. Munari, U., Henden, A., Vallenari, A., Bond, H. E., Corradi, R. L. M., Crause, L., Desidera, S., Giro, E., Marrese, P. M., Ragaini, S., Siviero, A., Sordo, R., Starrfield, S., Tomov, T., Villanova, S., Zwitter, T., Wagner, R. M., “On the distance, reddening and progenitor of V838 Mon”, Astron Astrophys, 434, 1107. 64. Oreiro, R., Pérez Hernández, F., Ulla, A., Garrido, R., Østensen, R., MacDonald, J., “Balloon 090100001: A short and long period pulsating sdB star”, Astron Astrophys, 438, 257. 65. Oreiro, R., Ulla, A., Pérez Hernández, F., MacDonald, J., Østensen, R., Rodríguez-López, C., “Balloon 09010001: Towards the White Dwarf Stage?”, ASP Conf Ser, 334, 631. 66. Østensen, R., Heber, U., Maxted, P., “Resolving sdB Binary Systems with Adaptive Optics”, ASP Conf Ser, 334, 435. 67. Palombara, N. L., Caraveo, P., Mignani, R., Hatziminaoglou, E., Bignami, G. F., Schirmer, M., “Multiwavelength Study of two Unidentified gamma-ray Sources”, Astrophys J Suppl, 297, 335. 68. Rix, S. A., Pettini, M., Leitherer, C., Bresolin, F., Kudritzki, R.-P., Steidel, C. C., “New Metallicity Diagnostics for High-Redshift Star-Forming Galaxies”, ASSL, 329, 311. 69. Pignata, G., Benetti, S., Buson, L., Hillebrandt, W., Leibundgut, B., Mazzali, P., Méndez, J., Patat, F., Ruiz-Lapuente, P., Stehle, M., Turatto, M., “Optical and Infrared Observations of SN 2002dj: a Twin of SN 2002bo”, ASP Conf Ser, 342, 266. 70. Rodríguez-Lopez, C., Ulla, A., Garrido, R., Manteiga, M., Casanova, V., Sota, A., Østensen, R., Oreiro, R., “Searching for Pulsations among sdOs”, ASP Conf Ser, 334, 627. 71. Rutten, R., “ING future: Prospects for the William Herschel Telescope”, Astronomy and Geophysics, 46, 9. 72. Sako, M., et al. (with Méndez, J.), 2005, “Early Results from the SDSS-II Supernova Survey”, American Astronomical Society Meeting Abstracts, 207. 84 • ING BIENNIAL R EPORT 2004–2005 73. Sánchez, S. F., Becker, T., Garcia-Lorenzo, B., Benn, C. R., Christensen, L., Kelz, A., Jahnke, K., Roth, M. M., “The merging/AGN connection. II. Ionization of the circumnuclear regions”, Astron Astrophys, 429, L21. 74. Schönberner, D., Jacob, R., Steffen, M., Perinotto, M., Corradi, R. L. M., Acker, A., “The evolution of planetary nebulae. II. Circumstellar environment and expansion properties”, Astron Astrophys, 431, 963. 75. Schmidt, G. D., Szkody, P., Homer, L., Smith, P. S., Chen, B., Henden, A., Solheim, J.-E., Wolfe, M. A., Greimel, R., “Unraveling the Puzzle of the Eclipsing Polar SDSS J015543.40+002807.2 with XMM and Optical Photometry/Spectropolarimetry”, Astrophys J, 620, 422. 76. Schwarz, H., Bendersky, C., Corradi, R., “Spectropolarimetry of the rings in NGC6543”, American Astronomical Society Meeting Abstracts, 207. 77. Todd, I., Pollacco, D., Skillen, I., Bramich, D. M., Bell, S., Augusteijn, T., “A survey of eclipsing binary stars in the eastern spiral arm of M31”, MNRAS, 362, 1006. 78. Torres, M. A. P., Steeghs, D., Greimel, R., Augusteijn, T., “Swift XRT position for XTE J1739-285”, The Astronomer's Telegram, 602, 1. 79. Trundle, C., Lennon, D. J., “Understanding B-type supergiants in the low metallicity environment of the SMC II”, Astron Astrophys, 434, 677. 80. Urbaneja, M. A., Herrero, A., Kudritzki, R.-P., Najarro, F., Smartt, S. J., Puls, J., Lennon, D. J., Corral, L. J., “Blue Luminous Stars in Nearby Galaxies: Quantitative Spectral Analysis of M33 B-Type Supergiant Stars”, Astrophys J, 635, 311. 81. Vauclair, G., Solheim, J.-E., Østensen, R. H., “Abell 43, a second pulsating “hybrid-PG 1159'' star”, Astron Astrophys, 433, 1097. 82. Witham, A., Knigge, C., Drew, J., Groot, P., Greimel, R., Parker, Q., “Discovering Interacting Binaries with Hα Surveys”, AIP Conf Proc, 797, 643. 83. Wright, S. A., Corradi, R. L. M., Perinotto, M., “Absolute spectrophotometry of northern compact planetary nebulae”, Astron Astrophys, 436, 967. 84. Ziffer, J., Campins, H., Licandro, J., Fernandez, Y. R., Bus, S., “Near-infrared Spectra of Two Asteroids with Low Tisserand Invariant”, AAS/Division for Planetary Sciences Meeting Abstracts, 37. ING BIENNIAL R EPORT 2004–2005 • 85 Appendix G SEMINARS Date Title Speaker University / Institution 2004 3 Feb LAMOST Telescope and Instrumentation: Concept, Technologies and Progress D. Yang Nanjing Institute of Astronomical Optics and Technology 20 Feb Circumstellar Matter in PNe and Other Evolved Stars H. E. Schwarz CTIO-NOAO-AURA 4 Mar Search for extrasolar planets with SARG S. Desidera Padova Observatory 12 Mar Planetary Nebulae in the Local Group L. Magrini Dipartimento di Astronomia e Scienza dello Spazio, University of Firenze 6 Apr Helium-rich subdwarf B stars: binaries, mergers or bizarre? A. Ahmad Armagh Observatory 7 Apr SuperWASP: The Super Wide Angle Search for Planets D. Pollacco Queen’s University of Belfast 15 Apr Basaltic Asteroids R. Duffard Observatorio Nazional de Rio, Brasil 21 Apr Observing Galaxy Haloes A. Romanowsky University of Nottingham 2 Jul SALT: 6 months to go! P. Charles University of Southampton 7 Jul Planetary transits and stellar variability S. Aigrain IoA, Cambridge 30 Jul What’s the role of environment on galaxies? P. Focardi Dipartimento di Astronomia, Università di Bologna 10 Aug Gamma Ray Bursts in the SWIFT Era A. Antonelli INAF-Osservatorio Astronomico di RomaItaly 22 Nov Physical Studies of Minor Bodies S. Fornasier Astronomy Dep. of Padova University 1 Dec Hot Stellar Populations in Galactic Globular Clusters: The population(s) S. Cassisi Osservatorio Astronomico di Collurania in puzzle goes deeper Teramo 2005 18 Feb The SOAR telescope is nigh ! H. Schwarz CTIO/NOAO/AURA 17 Mar Population of variable stars in the dwarf irregular galaxy NGC6822 L. Baldacci Osservatorio Astronomico di Bologna 5 May Asteroid Families: A new analysis T. Mothe Diniz Paris Observatory, Meudon 20 Jun The AstroGrid Virtual Observatory System: Release 1.0 N. Walton IoA, Cambridge & Astrogrid Consortium 8 July Is Scintillation the key to an improved ICRF? R. Ojha Australia Telescope National Facility, CSIRO 26 Aug OB associations in the era of planet formation T. Naylor School of Physics, University of Exeter 7 Sep Extreme clumping in the winds of Luminous Blue Variables B. Davies Dept. of Physics & Astronomy, Univ. of Leeds 23 Sep Old open clusters as tracers of galactic chemical evolution A. Bragaglia INAF-Osservatorio Astronomico di Bologna 13 Oct Remote observations with the NOT at the Nordic- Baltic summer school J.-E. Solheim Institute of Theoretical Astrophysics, Oslo in August 2005 24 Oct Features and performance of the Copenhagen generation 3 array-controller P. Nørregaard Copenhagen University Observatory 14 Nov New developments in CCD technology S. Tulloch ING 86 • ING BIENNIAL R EPORT 2004–2005 Appendix H FINANCIAL STATEMENT Financial year 2004/05 saw a continuation in the reduction of the UK’s contribution to ING operations as planned for under PPARC’s restructuring plan for ground based facilities. This was a result of the UK’s membership of the European Southern Observatory (ESO) and the consequent need to make savings in other parts of the UK’s ground based programme. Nevertheless, the overall financial position for the observatory was healthy and enabled not only a full operational programme to be carried out but also an interesting programme of enhancement and development projects. However, it should be noted that, as part of the restructuring plan, the 1.0m Jacobus Kapten Telescope (JKT) had been withdrawn from service in semester 2003B. The approved funding for ING’s Joint Programme during financial year 2004/05 provided a requisitions budget of € 3317k, including receipts for repayment services provided to other observatories at the Roque de Los Muchachos Observatory (ORM). As a result of careful financial management, the observatory managed to hold back approximately € 600k. This money was "banked" with PPARC to be called forward in the future to help offset the significant budgetary reductions planned from 2005 onwards. The resulting allocations and associated expenditure are set out below under the main budget headings (staff costs associated with the international posts at ING are excluded). Financial year 2004/2005 Budget centre Allocation € k Expenditure € k Operations Administration and management 112.1 90.5 Astronomy support 71.1 67.0 Conferences 5.0 0.8 Engineering support 388.0 340.2 Local staff 1154.0 1157.0 ORM operations 613.5 659.7 Sea-level infrastructure and services 225.0 192.2 Students 21.0 16.2 SUBTOTAL 2589.8 2524.5 Enhancements and developments 358.0 157.9 TOTAL 2947.5 2682.4 Financial year 2005/06 saw the final phase of the planned reduction of the UK’s contribution to ING's budget. As a result, the funds approved by the international partners through the ING Board totalled € 2149.5k. The observatory therefore requested the first portion, € 365k, of the "banked" funds be carried forward. This addition, plus funds received from the EU and repayment services mean that the total cash budget available increased to € 2769.5k. In addition, during the year, it became clear that there would be sizable underspend against UK staff costs and € 350k were therefore transferred from this budget to requisitions.This was distributed between the various activities as set out below. Due to delays in the delivery of goods and equipment, the year closed with approximately € 140k unspent, although this sum had been fully committed. Details of the expenditure between the various activities is also set out in the table below. Financial year 2005/2006 Budget centre Allocation € k Expenditure € k Operations Administration and management 88.8 82.7 Astronomy support 40.0 41.0 Conferences 15.0 17.0 Engineering support 359.0 331.0 Local staff 1333.8 1344.0 ORM operations 647.3 743.4 Sea-level infrastructure and services 190.8 226.3 Students 21.7 19.9 SUBTOTAL 2696.5 2805.3 Enhancements and developments 404.8 158.4 TOTAL 3101.3 2963.7 ING BIENNIAL R EPORT 2004–2005 • 87 Appendix I COMMITTEE MEMBERSHIP Name Responsibility Institution ING BOARD Prof T van der Hulst (from 10.2005) Chairperson University of Groningen Prof J Drew (to 10.2005) Chairperson Imperial College London Dr P Crowther (from10.2004) University of Sheffield Dr G Dalton University of Oxford Dr R García López IAC Prof J Hough (from 10.2005) University of Hertfordshire Prof T Marsh (to 10.2004) University of Warwick Dr R Stark NWO Dr C Vincent PPARC Ms D Telfer Secretary PPARC DIRECTOR'S ADVISORY COMMITTEE Dr M McCaughrean Chairperson University of Exeter Dr M Balcells IAC Dr P A James Liverpool John Moores University Dr N Tanvir University of Hertfordshire Dr E Tolstoy University of Groningen ING TIME ALLOCATION GROUPS UK Panel for the Allocation of Telescope Time (PATT) Dr R D Jeffries (from09.2004) Chairperson University of Keele Prof C Tadhunter (to 08.2004) Chairperson University of Sheffield ING TAG Dr D Pollacco (from semester 2005B) Chairperson Queen’s University of Belfast Dr R Oudmayer (to semester 2005B) Chairperson University of Leeds Dr O Almainy (to semester 2005B) University of Nottingham Dr J Baker (to semester 2005B) University of Oxford Dr M Jarvis (from semester 2005B) University of Oxford Dr C Knigge (from semester 2005B) University of Southampton Dr P Maxted (to semester 2005A) University of Keele Dr M Page (from semester 2005B) University College London Dr A Sansom (from semester 2004A) University of Central Lancashire Dr S Smartt (to semester 2004B) University of Cambridge Dr P Wheatley (from semester 2005A) University of Leicester Dr I Skillen Technical secretary ING NL ASTRON Programme Committee (PC) Prof M Franx (from 09.2005) Chairperson University of Leiden Dr H Röttgering (to 09.2005) Chairperson University of Leiden SP Comité de Asignación de Tiempos (CAT) Dr J A Belmonte (from 01.2004) Chairperson IAC Dr E Mediavilla (to 12.2003) Chairperson IAC 88 • ING BIENNIAL R EPORT 2004–2005 Appendix J ADDRESSES AND CONTACTS Isaac Newton Group of Telescopes (ING). Apartado de correos 321; E-38700 Santa Cruz de La Palma; Canary Islands; Spain; Tel: +34 922 425 400; Fax: +34 922 425 401. URL: http://www.ing.iac.es/ or http://www.ast.cam.ac.uk/ING/ (UK mirror). ING’s sea-level office: Mayantigo building; C/ Alvarez de Abreu, 70, 2nd floor; E-38700 Santa Cruz de La Palma; Canary Islands; Spain. ING at Roque de Los Muchachos Observatory: Tel: +34 922 405 500 (residence’s reception); +34 922 405 559 (WHT control room); +34 922 405 640 (INT control room); +34 922 405 585 (JKT control room). Name Telephone (+34 922) E-mail (@ing.iac.es) Director René Rutten 425 420 rgmr Head of Administration Les Edwins 425 418 lie Head of Astronomy Danny Lennon 425 440 djl Head of Engineering Gordon Talbot 425 419 rgt Head of Operations Kevin Dee 405 565 kmd Head of Computing Don Carlos Abrams 425 450 don Head of Telescope & Instrument Engineering Diego Cano 425 446 dcano Public Relations Javier Méndez 425 464 jma Telescope Scheduling Ian Skillen 425 439 wji Service Programme Pierre Leisy 425 441 service WHT Manager Chris Benn 425 432 crb INT Manager Romano Corradi 425 461 rcorradi Personnel Chelo Barreto 425 417 chelo Health and Safety Jürg Rey 405 632 juerg Freight Juan Martínez 425 414 juan Note: For updated ING contact information please visit http://www.ing.iac.es/About-ING/. Particle Physics and Astronomy Research Council (PPARC). Polaris House; North Star Avenue; Swindon SN2 1SZ; United Kingdom; Tel: +44 (0)1793 442 000; Fax: +44 (0)1793 442 002; URL: http://www.pparc.ac.uk/. Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO). P.O. Box 93138; 2509 AD Den Haag; The Netherlands; Tel: +31 (0)70 34 40 640; Fax: +31 (0)70 38 50 971; URL: http://www.nwo.nl/. Instituto de Astrofísica de Canarias (IAC). C/ Vía Láctea s/n; E-38200 La Laguna; Canary Islands; Spain; Tel: +34 922 605 200; Fax: +34 922 605 210; URL: http://www.iac.es/. Enquiries about the operation of the Roque de Los Muchachos Observatory can be made to the Instituto de Astrofísica de Canarias (IAC), see address above. Enquiries about observing time on the ING telescopes allocated by the Panel for the Allocation of Telescope Time (PATT) should be made to the executive secretary, PATT, at the PPARC address given above, or for Dutch time to the chairperson of the Programme Committee (PC), email: [email protected]. Enquiries about the share of time at the disposal of Spain should be made to the Comité para la Asignación de Tiempos (CAT), at the IAC address given above. Enquiries about the international time scheme should be made to the Secretary, CCI, at the IAC address given above. ING BIENNIAL R EPORT 2004–2005 • 89 Appendix K ACRONYMS AND ABBREVIATIONS AAO Anglo-Australian Observatory ASP Conf Ser Astronomical Society of the Pacific Conference Series Astron Astrophys Astronomy and Astrophysics Journal Astron Astrophys Suppl Astronomy and Astrophysics Journal Supplement Series Astron J Astronomical Journal Astron Soc Pac Conf Ser Astronomical Society of the Pacific Conference Series Astrophys J Astrophysical Journal Astrophys J Suppl Astrophysical Journal Supplement Series Astrophys Space Science Astrophysics and Space Science Journal AU Astronomical Unit (1.496×108 km) AUTOFIB Autofib Fibre Positioner AF2 Autofib Fibre Positioner Aux Auxiliary Port at the WHT Cassegrain focus Bull Am Astron Soc Bulletin of the American Astronomical Society Cass Cassegrain focus CAT Comité para la Asignación de Tiempos (Spanish panel for the allocation of telescope time) CCD Charge-Coupled Device CCI Comité Científico Internacional (International Scientific Committee) for Astrophysics CfA Harvard-Smithsonian Centre for Astrophysics CIRSI Cambridge Infra Red Survey Instrument DAS Data Acquisition System DIAS Dublin Institute for Advanced Studies DIMM Differential Image Motion Monitor ELECTRA Enhanced Light Efficiency Cophasing Telescope Resolution Actuator ESA European Space Agency ESTEC European Space Technology Centre Fib AUTOFIB fibre positioner FOS Faint Object Spectrograph FWHM Full Width Half Maximum GHRIL Ground Based High Resolution Imaging Laboratory GLAS Ground-layer Laser Adaptive optics System GRACE GRound based Adaptive optics Controlled Environment HST Hubble Space Telescope IAA Instituto de Astrofísica de Andalucía IAC Instituto de Astrofísica de Canarias IAU International Astronomical Union IAU Circ IAU Circular IAUNAM Instituto de Astronomía de la Universidad Nacional Autónoma de México IC Imperial College ICS Instrument Control System ICSTM Imperial College of Science, Technology and Medicine IDS Intermediate Dispersion Spectrograph IFCA Instituto de Física de Cantabria IMAFF Instituto de Matemáticas y Física Fundamental, Madrid INAOE Instituto Nacional de Astrofísica, Óptica y Electrónica, Mexico Inf Bull Variable Stars Information Bulletin on Variable Stars ING Isaac Newton Group ING Newsl ING Newsletter INGRID ING Red Imaging Device Int Astron Union Symp International Astronomical Union Symposium INT Isaac Newton Telescope INTEGRAL Integral field fibre feed for WYFFOS IoA Institute of Astronomy IR Infrared Irish Astron J Irish Astronomical Journal ISIS ISIS double spectrograph ITP International Time Programme JAG JKT Acquisition and Guiding Unit JKT Jacobus Kapteyn Telescope JOSE Joint Observatories Seeing Evaluation programme JSC Joint Steering Committee LAEFF Laboratory for Space Astrophysics and Fundamental Physics LDSS Low Dispersion Survey Spectrograph LIRIS Long-Slit Intermediate-Resolution Infrared Spectrograph 90 • ING BIENNIAL R EPORT 2004–2005 LJMU Liverpool John Moores University MARTINI Multi-Aperture Real Time Image Normalisation Instrument MCCD Mosaic CCD camera or National Astronomical Observatory of Japan camera MES Manchester Echelle Spectrograph Mem Soc Astron Ital Memorie della Società Astronomica Italiana MNRAS Monthly Notices of the Royal Astronomical Society MOMI Manchester Occulting Mask Imager MPIA Max Planck Institute of Astrophysics MSSL Mullard Space Science Laboratory MSSSO Mount Stromlo and Siding Spring Observatories Musicos Multi-SIte COntinuous Spectroscopy (fibre spectrograph on the INT) NAOMI Natural guide star Adaptive Optics system for Multiple-Purpose Instrumentation NBST National Board of Science and Technology of Ireland New Astron New Astronomy Journal New Astron Rev New Astronomy Review NRAL National Radio Astronomy Laboratory NWO Nederlandse Organisatie voor Wetenschappelijk Onderzoek OAN Observatorio Astronómico Nacional OASIS OASIS Integral Field Spectrograph OAT Observatorio Astronomico de Trieste ORM Observatorio del Roque de Los Muchachos (Roque de los Muchachos Observatory) OSCA OSCA Coronograph PASA Publications of the Astronomical Society of Australia PASP Publications of the Astronomical Society of the Pacific PATT Panel for the Allocation of Telescope Time PF Prime Focus PFC Prime Focus Camera PFIP WHT´s Prime Focus Imaging Platform Planet Space Sci Planetary and Space Science Journal PN.S Planetary Nebula Spectrograph PP People’s Photometer PPARC Particle Physics and Astronomy Research Council Proc Proceedings QMW Queen Mary and Westfield College QUB Queen’s University Belfast RBS Richardson-Brealy Spectrograph Rev Mex Astron Astrof Revista Mexicana de Astronomía y Astrofísica Rev Mex Astron Astrof Conf Ser Revista Mexicana de Astronomía y Astrofísica Series de Conferencias RGO Royal Greenwich Observatory RAL Rutherford Appleton Laboratory SAURON Spectrographic Areal Unit for Research on Optical Nebulae S-Cam Super-conducting Tunnel Junction Camera Space Sci Rev Space Science Reviews SPIE Society of Photo-Optical Instrumentation Engineers STScI Space Telescope Science Institute TAC Time Allocation Committee TAG Time Allocation Group TAURUS TAURUS Fabry-Perot spectrograph or imager TCS Telescope Control System TNG Telescopio Nazionale Galileo TRIFFID Galway/DIAS Image Sharpening Camera UCL University College London UCLAN University of Central Lancashire UCM Universidad Complutense de Madrid UES Utrecht Echelle Spectrograph UKIRT United Kingdom Infrared Telescope ULTRACAM Ultra-fast, triple-beam CCD camera WHIRCAM William Herschel Infrared Camera WFC Wide Field Camera WFS Wide Field Surveys with the WFC WHT William Herschel Telescope WYFFOS Wide Field Fibre Optics Spectrograph ZAMS Zero-Age Main Sequence ING BIENNIAL R EPORT 2004–2005 • 91 ISAAC NEWTON GROUP OF TELESCOPES (ING) Apartado de Correos 321 E-38700 Santa Cruz de La Palma Canary Islands SPAIN Tel: +34 922 425400 Fax: +34 922 425401 URL: http://www.ing.iac.es/